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╚═╝ ╚══════╝ ╚═╝ ╚═╝ ╚═╝╚═╝ ╚═╝PeTar is an N-body code specifically designed for modeling collisional stellar systems, where factors such as multiplicity (binaries, triples, etc.) and close encounters play a crucial role in dynamical evolution. PeTar offers several key advantages:
Precise gravitational force modeling: PeTar does not employ any softening of gravitational force, enabling accurate tracking of the orbital evolution of binaries, triples, and close encounters.
Incorporation of single and binary stellar evolution: Within the N-body simulation, PeTar dynamically evolves the masses, radii, and stellar types of individual stars. It also tracks significant events like supernovae, mass transfer, common envelope interactions, and binary mergers caused by stellar coalescence/collision and gravitational wave emission.
Galactic potential inclusion: PeTar allows for the simulation of tidal effects on stellar systems by incorporating the galactic potential.
Parallel computing capabilities: PeTar leverages multi-CPU processors/threads and GPU acceleration to accelerate simulations. This enables handling of over $10^7$ particles with a $100\%$ binary fraction.
Interoperability with other codes: PeTar can function as a module within other codes, facilitating the simulation of complex stellar environments. This includes compatibility with frameworks like AMUSE and SPH-based hydrodynamical code Asura-bridge.
The core N-body algorithm of PeTar encompasses three distinct methods, each tailored to the separation distance between individual pairs of particles (stars):
Barnes-Hut tree method: This technique, introduced by Barnes and Hut in 1986, is utilized for computing long-range forces between particles. These forces are then integrated using a second-order symplectic leap-frog integrator.
Fourth-order Hermite integrator with block time steps: PeTar employs this integrator, inspired by Aarseth's work in 2003, to precisely integrate the orbits of stars and the centers-of-mass of multiple systems. It is particularly effective for handling short-range forces.
Slow-down algorithmic regularization (SDAR) method: PeTar leverages the SDAR method, developed by Wang, Nitadori, and Makino in 2020, to integrate the dynamics of close-distance multiple systems. This is especially useful for scenarios involving hyperbolic encounters, binaries, and hierarchical few-body systems.
The core implementation of PeTar is predominantly in the C++ programming language. However, external modules within PeTar can be written in various programming languages.
The data analysis tool accompanying PeTar is developed in Python 3. Users are required to have a fundamental understanding of Python to effectively interact with the simulation data.
In particular, users are encouraged to familiarize themselves with key Python modules such as numpy, dict, and matplotlib. These modules encompass a wide range of functions essential for tasks like data reading, processing, and visualization.
This README document serves as a concise yet comprehensive guide detailing the installation and utilization of the code. It is strongly recommended that users thoroughly review this documentation before reaching out to the developers with any queries.
For a deeper understanding of the algorithms employed, additional details can be found in the work by Wang et al. (2020; available on arXiv: https://arxiv.org/abs/2006.16560). For developers seeking to understand the code structure, please consult the Doxygen documentation.
After completing the installation process, users can quickly get started by exploring three sample scripts located in the sample folder: star_cluster.sh, star_cluster_bse.sh, and star_cluster_bse_galpy.sh. These scripts provide practical demonstrations of simulating a star cluster using the PeTar code. They cover tasks such as generating initial conditions using mcluster, running simulations, and processing data to produce single and binary snapshots, core information, and Lagrangian radii. Here is a brief description of each script:
mcluster manual). This simulation uses only gravitational forces.Furthermore, users can access a Jupyter Notebook titled data_analysis.ipynb, which provides examples of data analysis in Python. By running one of the sample scripts, users can subsequently refer to the demonstrations in this notebook to analyze the simulation results. The data analysis module in PeTar offers greater convenience compared to manually parsing the output files. It is advisable to leverage this module instead of crafting reading code from scratch.
PeTar code is maintained across multiple branches, and for users seeking stability, it is advisable to obtain the released version. The master branch undergoes regular updates to introduce new features and address bugs. Users can opt for this version if they find the new features beneficial.
Other branches may not function correctly, and users are advised against interacting with them unless they have consulted the developer and comprehended the implementations and existing issues.
Users can retrieve the code version by running petar -h or using petar to start a simulation. The code version will be presented in the format [petar version][suffix]_[SDAR version], where:
[petar version] represents the commit count of the PeTar code.[SDAR version] indicates the commit count of the SDAR code.[suffix] signifies the development mode. If absent, it denotes the master version. If [suffix] is e or another term, it indicates an experimental or specialized version.The major modes are as follows:
The subsequent sections provide detailed explanations of the installation process and usage instructions. The final sections offer a brief overview of the methods employed in the code and introduce the AMUSE API.
petar.initpetar.find.itpetar.data.getherpetar.data.processpetar.get.object.snappetar.moviepetar.data.clearThis section describes how to install PeTar, including the required libraries and codes, the computer environment, and the installation options.
PeTar is built upon the FDPS and the SDAR codes. FDPS offers the particle-tree & particle-particle method and MPI and OpenMP parallelization. SDAR is an N-body code library that incorporates the slow-down algorithmic regularization and Hermite integrator for simulating the motion of particle clusters with short-range and close-distance interactions.
Please download the two codes from the following GitHub links:
FDPS: https://github.com/FDPS/FDPS (please use v6.0 or v7.0; v7.1 may not work)
The latest version of FDPS (v7.1) has a known issue that could lead to a crash of PeTar with an assertion error related to NaN check. After cloning FDPS from Git, in the FDPS directory, switch to the previous release v7.0 using the command:
git checkout v7.0To incorporate external galactic potentials in simulations, users can use the Galpy code through an interface integrated into PeTar. To use Galpy, users should install it either by executing
pip3 install --user galpyIn this scenario, PeTar can automatically detect Galpy.
If pip3 is unavailable, users can mamually download the source code from https://github.com/jobovy/galpy and specify the code path in the configure command (refer to the following guide).
If the source codes of these dependent libraries are located in the same directory as the PeTar directory, the configure script (see Section Compiling the code) can automatically detect them. Otherwise, users will need to specify their pathes by adding configure options:
./configure --with-[code_name_in_lower_case]-prefix=[code path] ...For example, if the PeTar, FDPS and SDAR codes are placed in the directory with pathes: /home/username/code/PeTar, /home/username/code/FDPS and /home/username/code/SDAR
the automatic detection will function.
In a different scenario, such as when Galpy is used but not installed via pip3 and the Galpy source code is located in /home/username/python/Galpy, users will have to specify its path using:
./configure --with-galpy-prefix=/home/username/python/Galpy ...To compile the code successfully, the C++ compiler (e.g., GNU gcc/g++, Intel icc/icpc, LLVM clang/clang++) must support at least the C++11 standard.
Using MPI necessitates the MPI compiler (e.g., mpic++). NVIDIA GPU and CUDA compiler are essential for GPU acceleration. SIMD support has been tested for GNU, Intel, and LLVM compilers. Since it hasn't been tested for others, it's recommended to use these three compiler types. The Fugaku ARM A64FX architecture is also compatible.
To use the SSE/BSE stellar evolution package, a Fortran (77) compiler, GNU gfortran, is required. It should be capable of providing an API to the C++ code, i.e., libgfortran is necessary. Intel ifort is currently not supported.
To use Galpy and the analysis tools, Python3 must be installed. Galpy also mandates the GSL library to be installed and detectable in the load library path.
All compilers should be accessible in the $PATH environment. For instance, to employ the OpenMPI C++ compiler, mpic++ needs to be available. This can be verified by entering mpic++ --version in the terminal, which should display the version of the current MPI C++ compiler. If the output indicates that the command is not found, users should install OpenMPI correctly.
Generally, the supercomputer offers various compiler options, such as different versions of Intel and GNU compilers. Before installing PeTar, users should ensure they correctly set up the compilers by reviewing the manual or consulting the supercomputer administrators.
Once the required libraries such as FPDS and SDAR are accessible, go to the PeTar directory and run the following command:
[environment variables] ./configure [options]This command will examine the local environment, automatically identify the compilers and features, with [environment variables] and [options] representing additional options to manage the features. Upon completion of the configuration process, a summary log will be displayed. It is important to review this log carefully to correctly choose the environment variables and options, including the paths for dependent libraries and compilers.
To view the available environment variables and options for configure, use the following command:
./configure -hA few useful environment variables and options are presented as follows:
To specify a custom installation path, use the following command:
./configure --prefix=[Installation path]The default installation path set by the configure script is /user/local, which requires administrator permission to access. It is not recommended to install PeTar there unless all users on the machine need to use the PeTar code. To install the code in a different location, users can add the --prefix option. For example, to install the code in /home/username/tools, users can include the option in the configure command:
./configure --prefix=/home/username/toolsIf PeTar has been previously installed and the executable file (petar) is already in the $PATH environment, configure will automatically use the same directory for installation.
To enable or disable MPI parallelization, use the following command:
./configure --with-mpi=[choices] where [choices] can be auto, yes, or no:
By default, configure will detect the C++, C, and Fortran compilers in the $PATH environment. If users prefer to manually specify these compilers, they can modify the environment variables CXX, CC, and FC accordingly. For instance, if users wish to use Intel C++ and C compilers with Intel MPI, they can use the following command:
CXX=mpiicpc CC=mpiicc ./configureHere, mpiicpc represents the Intel C++ MPI compiler, and mpiicc denotes the Intel C MPI compiler. If these compilers are not in the $PATH environment, users must provide the full path, as illustrated below:
CXX=/home/username/tool/bin/mpiicpc CC=/home/username/tool/bin/mpiicc ./configureIn this example, the Intel MPI compilers are installed in /home/username/tool/bin/.
For Mac OS users, clang, clang++, and flang compilers can be used instead of GNU compilers, as illustrated below:
CXX=clang++ CC=clang FC=flang ./configureBy default, PeTar enables multi-threaded OpenMP parallelization. To disable OpenMP, use the following command:
./configure --disable-openmpPeTar can utilize SIMD-like instructions to optimize the performance of tree force calculation and tree neighbor counting. The currently supported CPU architectures for enabling this feature are Intel/AMD x86 and Fugaku ARM A64FX. Users can specify the architecture using the following command:
./configure --with-arch=[choices]where [choices] include x86 and fugaku:
Please note that on the Fugaku supercomputer, the configuration only applies to the active nodes. Users are advised to initiate an interactive job to configure and compile the code.
PeTar supports multiple SIMD versions to enhance the performance of tree force calculation and tree neighbor counting. Users can choose the SIMD version using the following command:
./configure --with-simd=[choices]where [choices] can be auto, avx, avx2, or avx512, with the latter offering the highest speed:
Please note that the supported SIMD options of the compiler and the running CPU may differ. Make sure to use the SIMD version supported by the running CPU.
In the case of a supercomputer, the host and computing nodes might feature distinct CPU architectures. The configure script detects the SIMD version based on the local CPU. It is advisable to verify whether the CPU instructions on the computing node support a superior SIMD choice and opt for that during compilation.
PeTar supports the utilization of GPUs based on the CUDA language to accelerate tree force calculations as an alternative speed-up method to SIMD acceleration. To enable this feature, use the following command:
./configure --enable-cudaBy default, the GPU is not utilized. To enable it, ensure that NVIDIA CUDA is installed and compatible with the C++ compiler.
If the code crashes or a bug is present, users can enable the debugging mode as follows:
./configure --with-debug=[choices]where [choices] can be assert, g, or no:
Users can enable stellar evolution for stars and binaries using the following command:
./configure --with-interrupt=[choices]where [choices] include bse, mobse, and bseEmp.
In this option name, 'interrupt' refers to the N-body integration being interrupted by external effects on particles.
There are currently three options for stellar evolution packages based on SSE/BSE (Hurley et al. 2000, MNRAS, 315, 543; 2002, MNRAS, 329, 897):
It is important to mention that while all SSE/BSE package names only contain 'bse', the SSE package is also encompassed within them. From now on, the SSE/BSE based package will be denoted in a universal form as '[bse_name]'.
Enabling this option will also compile and install the standalone tool _petar.[bsename]. This C++ based tool calls stellar evolution functions to evolve single and binary stars to a specified age and metallicity. OpenMP parallelization is utilized to accelerate calculations when handling a large group of stars and binaries.
To use the extreme metal-poor evolution track of bseEmp, users must create a symbolic link in the working directory to either the ffbonn or ffgeneva directory located in 'PeTar/bse-interface/bseEmp/emptrack/', depending on the selected stellar evolution track mode during the execution of PeTar. Failure to do this will lead to a file I/O error, causing the simulation to crash.
When utilizing SSE/BSE packages, users can control whether to activate stellar evolution during the simulation using the petar option --stellar-evolution and --detect-interrupt for single and binary evolution, respectively. When --stellar-evolution 2 is specified, dynamical tide for binary stars and hyperbolic gravitational wave energy/angular momentum loss for compact binaries are enabled. It's worth noting that the dynamical tide is still an experimental feature, and its results may not always be physically accurate. By default (--stellar-evolution 1), dynamical tide remains inactive.
Users can incorporate external potential and force into particles by utilizing the following command:
./configure --with-external=[choices]Currently, [choices] offers only one option: galpy. Additional options will be introduced in future versions.
The Galpy library is an external potential library based on Python and C, offering a wide range of potential choices. It allows for the flexible combination of multiple potentials (requiring the use of the Galpy Python interface to instantiate, as detailed in their documentation).
Enabling this option will also compile and install the standalone tools petar.galpy and petar.galpy.help:
petar.galpy is a straightforward tool that utilizes the Galpy C interface to compute acceleration and potentials for a particle list using a specified potential model.petar.galpy.help is a Python script tool designed to assist users in generating input options for potential models. When designing a specific potential using the Galpy Python interface, this tool also offers a function to convert a Galpy potential instance into an option or a configuration file used by PeTar.When combining multiple options, they should be used together, as shown in the example below:
./configure --prefix=/opt/petar --enable-cudaThis command will install the executable files in /opt/petar (this directory requires root permission) and activate GPU support.
After configuring, execute the following commands:
make
make installto compile and install the code.
The executable files, petar and petar.[tool name], will be installed in [Install path]/bin.
petar serves as the primary routine for conducting N-body simulations. It is essentially a symbolic link to petar.**, with the suffix reflecting the code's features based on the configuration, such as petar.avx2.bse.petar.[tool name] comprises a set of tools for debugging, initializing data files, optimizing performance, and analyzing data. Detailed information can be found in the section Useful tools. For each tool, running petar.[tool name] -h will display all available options along with descriptions. Users are advised to refer to this first to ensure correct tool usage.If [Install path]/bin is added to the environment variable $PATH, the executable files can be directly accessed from any directory in the Linux system using the following command:
export PATH=$PATH:[Install path]/binAnalysis of simulation-generated data files can be performed using the Python3-based data analysis module located in [Install path]/include/petar. To import the code, include [Install path]/include in the Python include path (the environment variable $PYTHONPATH) with the following command:
export PYTHONPATH=$PYTHONPATH:[Install path]/includeThese environment variable configuration commands need to be executed each time a new terminal is opened. To automate the loading of these variables, it is advisable to add these commands to the .bashrc file in the case of a bash Linux system.
PeTar is capable of conducting $N$-body simulations and offers a range of tools for tasks such as initializing input files, post-processing to calculate Lagrangian radii, core radius determination, binary, triple, and quadruple detection, movie creation, and a Python package for data analysis. This section provides a detailed overview of these features.
To initiate an $N$-body simulation, users must provide the initial conditions of the particle system. Various tools are available for generating initial conditions, such as MCluster and AMUSE.
The initial conditions are stored in a data file with a format that consists of 7 columns representing the masses, positions, and velocities of each particle per line.
Subsequently, users can utilize the petar.init tool (refer to Initial Input Data File) to convert this data file into a snapshot file following the petar style.
The process of starting an $N$-body simulation using the petar command depends on whether MPI and OpenMP support are compiled.
In the straightforward scenario, the standard procedure for commencing an $N$-body simulation is as follows:
petar [options] [snapshot filename]Here, [snapshot filename] represents the filename of a snapshot of the particle system at a specific time, and [options] are utilized to regulate the behaviors of the simulations (refer to Options).
For a new simulation, the snapshot file stores the initial conditions of a particle system. The file can be generated from the petar.init tool. For a restarted simulation, this file is the outputted snapshot from a previous simulation.
When OpenMP is employed, to prevent segmentation faults in simulations with a large number of particles, users need to set the environment variable OMP_STACKSIZE to a sufficiently large value. For instance:
export OMP_STACKSIZE=128MFurthermore, ensure that the maximum stack size is unlimited by executing the command ulimit -s. It should return 'unlimited'. If not, run ulimit -s unlimited before using petar.
The default number of threads is the maximum number supported by the host machine. Users can specify the number of threads (N_threads) by setting the environment variable OMP_NUM_THREADS. To enhance performance, N_threads should generally be kept at or below 8.
These environment variables can be utilized when executing petar, as shown in the following example:
OMP_STACKSIZE=128M OMP_NUM_THREADS=8 petar [options] [snapshot filename]A convenient approach is to set OMP_NUM_THREADS, OMP_STACKSIZE, and ulimit -s in the initial script file of the terminal, such as the .bashrc file for a Bash system:
export OMP_STACKSIZE=128M
export OMP_NUM_THREADS=N_threads
ulimit -s unlimitedSubsequently, when a terminal is opened or source ~/.bashrc is executed in an existing terminal, these lines will be automatically executed. In this scenario, there is no need to specify OMP_STACKSIZE=128M OMP_NUM_THREADS=N_threads when using the petar command.
When utilizing OpenMP, it is important to note that the simulation may not be reproducible, as dynamic parallelism is employed to integrate the short-range interactions.
When MPI is utilized, an MPI launcher is required to utilize multiple MPI processors. The standard approach is as follows:
mpiexec -n [N_mpi] petar [options] [snapshot filename]Here, [N_mpi] denotes the number of MPI processors.
For optimal performance, OpenMP and MPI can be used together. In the example below, 4 MPI processors and 8 threads per processor are employed:
OMP_STACKSIZE=128M OMP_NUM_THREADS=8 mpiexec -n 4 petar [options] [snapshot filename]It is important to ensure that N_mpi x N_threads is less than the total available CPU threads in the computing facility.
Please note that on a supercomputer, the MPI launcher may not be named mpiexec, and the method for setting the number of OpenMP threads may vary. Refer to the documentation of the job system or consult with the administrator to determine the appropriate approach for using MPI and OpenMP in that specific environment.
When GPU support is enabled, each MPI processor will initiate one GPU job. Modern NVIDIA GPUs can handle multiple jobs simultaneously.
Therefore, it is acceptable for N_mpi to exceed the number of GPUs available. However, if N_mpi is too large, the GPU memory may become insufficient, leading to a Cuda Memory allocation error. In such cases, utilizing more OpenMP threads and fewer MPI processors is a preferable approach.
In scenarios where multiple GPUs are present, each MPI processor will utilize a different GPU based on the processor and GPU IDs. If users wish to exclusively utilize a specific GPU, they can employ the environment variable CUDA_VISIBLE_DEVICES=[GPU index]. For instance:
CUDA_VISIBLE_DEVICES=1 petar [options] [particle data filename]This command will utilize the second GPU in the system (indexing starts from 0). The CUDA_VISIBLE_DEVICES environment variable can also be configured in the initial script file of the terminal.
Any snapshot of particle data generated during a simulation can be utilized to resume the simulation at a specific time. To resume the simulation with the same parameter configuration as before, use the following command:
petar -p input.par [options] [snapshot filename]Here, input.par stores the previous parameter choices used in a simulation, automatically generated from the prior simulation.
It is possible to modify the options for resumed simulations in two ways. Users can either directly modify input.par to adjust parameters before resuming or specify new parameters in [options] within the petar command mentioned earlier. It is crucial to place [options] after -p input.par to prevent them from being overwritten by the parameters stored in input.par. For instance, to update the end time of the simulation to 10 after resuming simulations from the snapshot file data.5, use the following command:
petar -p input.par -t 10 data.5 By default, after resuming, the snapshot files with the same name will be replaced. However, for other output files, new data will be appended to the existing ones (e.g., filenames with suffixes like esc, group, etc.).
In cases where a previous simulation did not reach completion and terminated abnormally, resuming the simulation from the last snapshot file may result in some events being repeated in the output data files. For instance, the same stellar evolution event might be recorded twice in a file with the '.sse' suffix. Similar behavior may occur when restarting the simulation from a non-final snapshot.
To prevent duplicate events, users can utilize petar.data.clear to remove events with recorded times greater than a specified time criterion before resuming. However, caution should be exercised to avoid deleting useful data inadvertently.
To overwrite the output files instead of appending to them, the option -a 0 can be included in the petar command.
Users have the ability to specify various parameters in the options of the petar command to control aspects such as the number of binaries, time steps, energy error criteria, and more. There are two types of options available: single-character options starting with '-' and long options starting with '--'. It is advisable for users to initially review all single-character options listed by running petar -h. Here are some useful options:
-u: Sets the unit system for input data. Using -u 1 requires the initial snapshot data to be in units of Msun, pc, and pc/Myr. Otherwise, the gravitational constant (G) is assumed to be 1 (Henon unit). It's essential to ensure consistency in unit settings when utilizing the petar.init tool. petar does not scale units, only modifying the gravitational constant. The -u 1 option sets the value of G in the unit set of [Msun, pc, myr], and adjusts unit scaling factors when using stellar evolution and galactic tidal field.
-t: Specifies the finishing time. Note that the tree time steps used in petar are integer powers of 0.5. If the finishing time does not be a multiple of the tree time step (as specified by the -s option), the simulation may not end precisely at the specified time.
-o: Sets the time interval for outputting data (snapshots and status). This interval should also be a multiple of the tree time step.
-s: Determines the tree time step, which should be an integer power of 0.5. When set, the changeover radius is automatically calculated unless -r is manually specified.
-r: Defines the outer boundary of changeover radii. When set, the tree time step is automatically determined.
-a: Controls data appending. Using -a 1 (default) appends new data to existing files after a restart, while other values rewrite the files. Exercise caution when restarting simulations with this option.
-b: Specifies the initial number of binaries. This is crucial for accurate velocity dispersion calculation, which in turn affects the automatic determination of tree time step and changeover radii. Primordial binaries should be listed first in the input data file (two neighbor lines per pair).
-w: Sets the output style. With -w 2, all particle data is printed in a single line along with system status information per output time, which can be beneficial for data analysis with small N.
-i: Determines the format of snapshot data, allowing for BINARY or ASCII format selection.
-G: Specifies the gravitational constant.
It is important to note that -s and -r significantly impact simulation accuracy and performance. Users should exercise caution with these options. The petar.find.dt tool can assist in finding optimized values for star clusters. For a comprehensive understanding and improved configuration, users may need to refer to the reference paper.
When using stellar evolution packages (e.g., BSE) and external potentials (e.g., Galpy), corresponding options are also displayed in petar -h.
The performance of PeTar is influenced by several crucial parameters and is also dependent on the initial conditions of particle (stellar) systems. To achieve optimal performance for a given input model, users must carefully adjust the following parameters:
petar option -sThe tree time step represents a fixed time interval for computing the long-range (particle-tree) force. Calculating the long-range force is computationally intensive, with a complexity of $O(N \log N)$. Therefore, a smaller time step results in more computationally expensive calculations per unit of physical time. However, it's essential not to increase the tree time step excessively, as discussed further regarding the changeover and neighbor searching radii.
petar option -rThe changeover region denotes the overlapping shell between long-range and short-range interactions. Below the inner region, short-range interactions are computed using 4th-order Hermite integration with individual time steps and the SDAR method. Above the outer region, long-range interactions are calculated using 2nd or 4th-order LeapFrog integration with the particle-tree method. In the intermediate region, both short- and long-range interactions are considered. The inner and outer radii are mass-weighted (m^(1/3)) for each particle, with the default ratio set at 0.1 (via the petar option --r-ratio).
Consistency between changeover radii and tree time steps is crucial to ensure accurate simulation results (refer to the PeTar paper for detailed information). A straightforward way to grasp this concept is by examining a circular Kepler orbit of two particles with a semi-major axis within the changeover region. Inside this region, the forces between the particles are divided into short-range and long-range components. Short-range forces are recalculated at each Hermite time step, while long-range forces are computed at every tree time step. Since the Hermite time step is smaller than the tree time step, the long-range forces impart velocity adjustments to the particles after several Hermite time steps. If the tree time step is too large, with only a few steps per Kepler orbit, the time resolution of long-range forces or velocity adjustments becomes insufficient, leading to inaccurate orbit integration (resulting in non-Keplerian orbits). Therefore, once the changeover region is defined, the tree time step should be sufficiently small to ensure at least several tens of sampling points for calculating the long-range forces (velocity adjustments) along the Kepler orbit.
In the absence of explicitly specified -s and -r values, petar automatically determines the tree time step and changeover radii based on the assumption that the input model represents a spherically symmetric star cluster with a King or Plummer-like density profile. For more intricate input models lacking a spherical structure, these parameters may require manual determination or the utilization of the option --nstep-dt-soft-kepler, following the self-consistent rule (tree time step - changeover radius relation) as exemplified in the aforementioned Kepler orbit scenario.
petar option --r-search-minThe changeover region delineates the boundary between short- and long-range interactions. In PeTar, an additional neighbor searching radius is defined for each particle to identify neighboring candidates expected to be within the changeover region during the subsequent tree time step. The minimum searching radius is slightly larger than the outer changeover radius, with the actual searching radius also depends on the particle's velocity. As a particle's velocity increases, it can cover a greater distance within a single tree time step, necessitating a larger searching radius. However, in cases where the velocity is excessively high, the searching radius may become too large. To address this issue, an additional mechanism is implemented to mitigate the number of neighbors: for every neighbor and the particle, a Kepler orbit assumption is made, and the peri-center distance is computed. If the peri-center lies outside a specified criterion, it is disregarded as a neighbor.
The neighbor searching radius is a crucial parameter that significantly impacts performance. For parallel computing of short-range integration, PeTar initially employs the neighbor searching radius to assemble nearby particles into individual clusters. Each cluster assigns only one CPU core for the short-range (Hermite+SDAR) integration in the following tree time step. The clustering algorithm ensures that all neighbors of each cluster member are also within the same cluster. Excessive neighbor radii can lead to the formation of a single massive cluster encompassing most system particles, resulting in one CPU core handling this cluster while others remain idle. This imbalance in workload undermines computational efficiency and can notably reduce performance. Consequently, the neighbor searching radius for each particle system should not be excessively large.
Upon determining the changeover radius (-r), petar automatically computes the neighbor searching radius. If users prefer manual determination of the neighbor searching radius, the following options can be configured:
--r-search-min: establishes the minimum neighbor searching radius reference, with the final radius also mass-weighted, akin to the changeover radius.--search-peri-factor: sets the maximum peri-center criterion assuming two neighbors possess a Kepler orbit.--search-vel-factor: determines the velocity-dependent addition to the neighbor radius (base neighbor radius + coefficient velocity tree time step).petar option --r-binThe third pivotal radius influencing performance is the radius used to identify a multiple group where the SDAR method is applied. In dense stellar systems, multiple groups like binaries, triples, and quadruples frequently occur, exhibiting significantly shorter orbital periods for inner members compared to single stars orbiting within the host particle system. The SDAR method in PeTar plays a crucial role in ensuring accuracy and efficiency in integrating their orbits, with binary stellar evolution also addressed within the SDAR method. The criterion for selecting group members is the group radius (--r-bin), which is automatically determined based on the changeover inner radius. If this radius is excessively large, the SDAR method becomes resource-intensive due to an excessive number of selected members in a multiple group. Conversely, if the radius is too small, some binaries may not be integrated accurately, as the Hermite integrator exhibits a systematic long-term drift of energy and angular momentum for periodic motion.
When initiating a new simulation, the automatically determined tree time step and radii may not always be the optimal choice for users. To select the most suitable tree time step, users can utilize the petar.find.dt tool (refer to Find tree time step). This tool is compatible only with PeTar's autodetermined tree time step and changeover radii (refer to Outer Changeover Radius).
In cases where the structure of the particle system undergoes significant evolution over an extended period, users may wish to adjust the tree time step and radii mentioned earlier to enhance performance. If users prefer to modify only the tree time step while allowing petar to determine the radii automatically, the options in the following example are necessary to restart the simulation:
petar -p input.par -s [new tree_time_step] -r 0 --r-search-min 0 --r-bin 0 [other options] [snapshot filename for restart]Here, -r 0 --r-search-min 0 --r-bin 0 are employed to reset all three radii and activate autodetermination based on the new tree time step. Users can also employ petar.find.dt to select the optimal restart tree time step (refer to Find tree time step).
When petar is running, several pieces of information are displayed at the beginning:
The FDPS logo and PeTar details are printed as follows, showcasing copyright information, versions, and references for citation.
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|| Framework for Developing ||
|| Particle Simulator ||
|| Version 7.0 (2021/08) ||
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...Enabled features (selected during configuration), such as stellar evolution packages, external packages, and GPU utilization, are listed:
Use quadrupole moment in tree force calculation
Use 3rd order tidal tensor method
...Any modified input parameters are displayed when using corresponding petar options.
Input data unit, 0: unknown, referring to G; 1: mass:Msun, length:pc, time:Myr, velocity:pc/Myr: 1
Number of primordial binaries for initialization (assuming the binaries ID=1,2*n_bin): 500
...Unit scaling for PeTar, stellar evolution packages (e.g., SSE/BSE), and external packages (e.g., Galpy) is outlined.
----- Unit set 1: Msun, pc, Myr -----
gravitational_constant = 0.0044983099795944 pc^3/(Msun*Myr^2)
----- Unit conversion for BSE -----
tscale = 1 Myr / Myr
mscale = 1 Msun / Msun
rscale = 44353565.919218 Rsun / pc
vscale = 0.9778131076864 [km/s] / [pc/Myr]A brief parameter list for tree time step and key radii influencing performance is provided.
----- Parameter list: -----
Average mass = 0.52232350485643
Mean inner changeover radius = 0.0021228717795716
Mean outer changeover radius = 0.021228717795716
Mean SDAR group detection radius = 0.0016982974236573
Minimum neighbor searching radius = 0.024787679043148
Velocity dispersion = 0.60739605289507
Tree time step = 0.001953125
Output time step = 1The definitions of these parameters are as follows:
Average mass: average mass of all objects.Mean inner changeover radius: mean inner changeover radius.Mean outer changeover radius: mean outer changeover radius.Mean SDAR group detection radius: the criterion for selecting SDAR group members.Minimum neighbor searching radius: the minimum neighbor searching radius reference.Velocity dispersion: velocity dispersion of the system.Tree time step: tree time step.Output time step: snapshot and status output time step.These parameters determine the performance of a simulation, see details in Performance Optimization.
If Galpy is utilized, the Galpy potential setup information may be printed.
Galpy parameters, time: 0 Next update time: 0
Potential set 1 Mode: 0 GM: 0 Pos: 0 0 0 Vel: 0 0 0 Acc: 0 0 0
Potential type indice: 15 5 9
Potential arguments: 251.63858935563 1.8 1900 306770418.38589 3000 280 1965095308.1922 16000In case the SSE/BSE-based stellar evolution package is employed, common block and global parameters are showcased.
----- SSE/BSE common block parameter list: -----
value1: neta: 0.50000000000000000 bwind: 0.0000000000000000 hewind: 1.0000000000000000
...Filenames for dumped input parameters are specified.
----- Dump parameter files -----
Save input parameters to file input.par
...By default, these include:
input.par: Input parameters of petar, useful for restarting the simulation from a snapshot.input.par.hard: Input parameters of the hard component (short-range interaction part; Hermite + SDAR), utilized for testing the dumped hard cluster with _petar.hard.debug_.input.par.[bse_name]: Parameters for the SSE/BSE-based package, necessary for restarting the simulation and for petar.hard.debug if an SSE/BSE-based package is used.input.par.galpy: Galpy parameters for simulation restart purposes.After the "Finish parameter initialization" line, the simulation status is updated at each output time interval (defined by the -o option). The status content follows a format similar to the example provided below:
Time, number of real particles, all particles (including artificial particles), removed particles, and escaped particles; both locally (within the first MPI process) and globally (across all MPI processes):
Example output information at time 1:
Time: 1 N_real(loc): 1378 N_real(glb): 1378 N_all(loc): 1378 N_all(glb): 1378 N_remove(glb): 0 N_escape(glb): 0Energy check: Two rows are printed. The first row displays physical energy, while the second row shows slow-down energy (referenced in the petar commander).
Energy: Error/Total Error Error_cum Total Kinetic Potential Modify Modify_group Modify_single Error_PP Error_PP_cum
Physic: 1.883442e-05 -644.6969 -644.6969 -3.422972e+07 1.846359e+07 -5.269331e+07 1841.216 0 0.008989855 -8.67599e-06 -8.67599e-06
Slowdown: 1.883442e-05 -644.6969 -644.6969 -3.422972e+07 1.846359e+07 -5.269331e+07 1841.216 0 0.008989855 -8.67599e-06 -8.67599e-06Angular momentum: Error at the current step, cumulative error, components in x, y, z directions, and value.
Angular Momentum: |L|err: 187484.2 |L|err_cum: 187484.2 L: -1.17383e+07 -1.20975e+07 -1.267862e+09 |L|: 1.267974e+09System total mass, center position, and velocity.
C.M.: mass: 736.5417 pos: 5127.807 -5729.159 7.270318 vel: -165.7037 -150.611 3.006304Performance information:
Tree step number: 512**** Wallclock time per step (local): [Min/Max]
Total PP_single PP_cluster PP_cross PP_intrpt* Tree_NB Tree_Force Force_corr Kick FindCluster CreateGroup Domain_deco Ex_Ptcl Output Status Other
0.009742 0.0006008 0.00016328 2.8949e-06 0 0.00069683 0.004435 2.6859e-05 3.3679e-05 8.365e-05 0.00011302 2.0602e-06 4.7604e-05 5.4633e-05 1.8945e-08 0.0034471
0.0097421 0.00060092 0.00016398 3.0875e-06 0 0.00070318 0.0044427 2.7012e-05 3.3787e-05 8.3776e-05 0.00011312 2.1375e-06 4.7723e-05 5.4636e-05 1.9141e-08 0.0034481**** FDPS tree soft force time profile (local):
Sample_ptcl Domain_deco Ex_ptcl Set_ptcl_LT Set_ptcl_GT Make_LT Make_GT SetRootCell Calc_force Calc_mom_LT Calc_mom_GT Make_LET_1 Make_LET_2 Ex_LET_1 Ex_LET_2 Write_back
0 0 0 5.2026e-05 1.7637e-06 0.00021123 7.0745e-05 8.7232e-06 0.0022072 4.4457e-05 0.0018011 1.3547e-05 0 4.401e-06 0 2.0096e-05**** Tree neighbor time profile (local):
Sample_ptcl Domain_deco Ex_ptcl Set_ptcl_LT Set_ptcl_GT Make_LT Make_GT SetRootCell Calc_force Calc_mom_LT Calc_mom_GT Make_LET_1 Make_LET_2 Ex_LET_1 Ex_LET_2 Write_back
0 0 0 3.6579e-05 1.6174e-06 0.00021966 7.2012e-05 7.7332e-06 0.00025779 3.126e-05 2.935e-05 2.6922e-05 0 1.4563e-06 0 1.2669e-05**** Number per step (global):
PP_single PP_cluster PP_cross PP_intrpt* Cluster Cross AR_step_sum AR_tsyn_sum AR_group_N Iso_group_N H4_step_sum H4_no_NB Ep-Ep_sum Ep-Sp_sum
1345.6 32.436 0 0 14.744 0 7.0586 4.0996 0 0 329.74 0 1.6972e+06 34134**** Number of members in clusters (global):
1 2 3 4 5 6
1345.6 13.24 0.68164 0.31055 0.40234 0.10938The performance information is crucial for verifying whether the simulation has been set up with appropriate tree time steps and radii parameters.
To ensure reasonable performance, the Tree_Force wallclock time should primarily contribute to the total time. If numerous multiple groups, such as primordial binaries, are present, PP_cluster may also consume time. However, if PP_cluster's time consumption is excessive (dominating most of the total time), users should consider adjusting the changeover radius, neighbor searching radius, and group radii (refer to Performance Optimization).
The histogram depicting the number of members in clusters is valuable for determining whether the neighbor searching radius is too large. In a low-density system, the maximum number of members should typically be around 20, as seen in the example provided (6). In a high-density system or a system with high-velocity particles, the maximum number may be higher. Nonetheless, if it remains within a few hundred members and the PP_cluster wallclock time is not excessively large, the setup is acceptable.
In addition to the printed information provided by the petar commander, there are several output files detailed in the table below:
| File name | Content |
|---|---|
| data.[index] | Snapshot files for each output time. The format mirrors that of the input data file. |
Users can reference the definitions of the first line (header) and columns using petar -h. |
|
| [index] denotes the output order, starting from 0 (initial snapshot). It does not correspond to time unless the output interval is set to 1. | |
| data.[index].randseeds | The random seeds for each OpenMP thread, used for restarting purposes. |
| data.esc.[MPI rank] | Contains information on escaped particles, with columns matching those in snapshot files, and an additional column for the escaped time at the beginning. |
| data.group.[MPI rank] | Provides details on the start and end of multiple systems (e.g., binary, triple ...) identified during SDAR integration. |
The definition of a multiple system is based on the distance criterion specified in the petar option --r-bin. |
|
| In cases where a multiple system spans multiple tree time steps, the start event may be recorded multiple times during each tree time step, while only one or no end event is recorded. This behavior is a result of the algorithm's design. | |
| data.status | Includes the evolution of global parameters such as energies, angular momentum, particle count, system center position, and velocity. |
When the petar option -w 2 is utilized, this file includes all particle information similar to the snapshot files. Instead of segregating particles into distinct lines, all particles are consolidated into a single line. |
|
| data.prof.rank.[MPI rank] | Offers performance measurements for various parts of the code throughout the simulation. |
When utilizing the SSE/BSE stellar evolution options (--with-interrupt during configure), additional files are generated:
| File name | Content |
|---|---|
| data.[sse_name].[MPI rank] | Contains records of single stellar evolution events, such as type changes and supernovae. Note that if a star evolves rapidly (less than the dynamical integration time step), internal type changes may not be captured. |
| data.[bse_name].[MPI rank] | Records binary stellar evolution events. All binary type changes are logged; however, if 'Warning: BSE event storage overflow!' appears during the simulation, it indicates that binary type changes are too frequent, resulting in some changes not being recorded for the corresponding binary. |
| When Galpy is employed (--with-external=galpy), under certain conditions, a galpy parameter file may be generated alongside each snapshot file: | File name | Content |
|---|---|---|
| data.[index].galpy | Contains the galpy parameter file for each snapshot, which may be necessary for restart purposes. |
In this context, 'data' serves as the default prefix for output files, although users have the flexibility to modify it using the petar option -f.
For instance, by specifying -f output, the output files will be named 'output.[index]', 'output.esc.[MPI rank]', and so forth.
The term [MPI rank] denotes the MPI processor responsible for outputting the data. Consequently, the number of data files with this suffix aligns with the count of MPI processors employed in the simulation. For instance, with two MPI processors, the escape data files will be labeled 'data.esc.0' and 'data.esc.1'.
Prior to accessing these files, it is advisable to execute the petar.data.gether tool to consolidate the individual files generated by different MPI ranks into a single file for ease of use.
The petar.data.gether tool not only consolidates files from various MPI processors but also generates new files accessible by the petar Python data analysis tool (refer to Python Data Analysis Module).
petar.data.gether separates few-body groups with varying member counts into individual files labeled with the suffix ".n[number of members in groups]".For a detailed overview of the files generated by petar.data.gether and the corresponding Python reading methods, refer to Gathering Output Files.
Given the extensive number of columns in each file, it is recommended to utilize the Python data analysis tool for data access. This tool simplifies the process of selecting specific parameters (columns) and conducting data operations (selection, calculation, and plotting), akin to using dict and numpy in Python.
Moreover, it helps prevent errors in column reading. Consequently, column definitions are not provided in the manual or within the file headers.
For column specifics, consult the documentation of the relevant analysis tool associated with each file.
The raw snapshot files do not encompass information on binaries or multiple systems. To identify and acquire details on Lagrangian and core properties, the petar.data.process tool can be employed (refer to Parallel Data Processing).
By default, petar outputs snapshots in ASCII format. The advantage of ASCII format is that users can directly read the file using a standard text reader. However, it is recommended to output snapshots in BINARY format by setting the -i option of petar. For instance,
petar -i 2 ...allows reading the input snapshot in ASCII format and outputting snapshots in BINARY format. BINARY format snapshots preserve precision for floating-point numbers, are significantly faster (at least 10 times faster) to read and write by petar and PeTar's data analysis module, and result in much smaller file sizes compared to ASCII format, helping to conserve hard disk space.
Users can also convert between ASCII and BINARY formats after simulations using the petar.format.transfer tool (refer to Data Format Conversion). Additionally, it is possible to convert post-processed files from petar.data.process using the petar.format.transfer.post tool.
There are 1-3 sets of units in petar depending on the packages utilized:
In the absence of additional stellar evolution and external potential packages, PeTar adheres to the units specified in the input files. Within the PeTar framework, there is no internal unit conversion. The only adjustable parameter is the gravitational constant, which can be modified to align with the units defined in the input data file (Refer to Options). Therefore, it is important that the input data maintains a consistent unit set: the velocity unit must correspond to the length unit. For instance, if the length unit is pc, the velocity unit should be pc/[time unit]. It is not permissible to use km/[time unit] as this would need an additional unit conversion from kilometers to parsecs during integration. Such conversions introduce unnecessary complexities and potential bugs without offering any tangible benefits. Consequently, PeTar restricts unit modifications to solely adjusting the gravitational constant to uphold a self-consistent unit system.
Given the absence of unit conversions, the output log, snapshot data (PeTar component), escaper files, and group files adhere to the unit set specified in the input data alongside the corresponding gravitational constant. For instance, if the input data utilizes units such as (Myr, pc, pc/Myr), the time and energy values in the output log will also be expressed in the same unit system. The potential energy calculations will account for the gravitational constant within this context.
The stellar evolution package (e.g., BSE) operates on a distinct unit system compared to PeTar. Consequently, there exists a unit conversion between the PeTar component and the stellar evolution package. Users can manually define the conversion scaling factors using petar options such as --bse-rscale (refer to petar -h for detailed information). It is advisable to adopt a unit set consistent with input data (e.g., in terms of solar masses, parsecs, and parsecs/Myr) to leverage the petar option -u 1, enabling automatic calculation of the conversion factor by PeTar. The unit system employed in the snapshot files for the stellar evolution segment and the output files "[data filename prefix].[s/b]se.[MPI rank]" align with the unit system specified in '[bse_name]'.
The external potential package (Galpy) introduces yet another unit system, necessitating a separate unit conversion between the PeTar component and Galpy. Users can manually define the conversion factors for Galpy using options like --galpy-rscale (refer to petar -h for specifics). To streamline the process and minimize complexities, it is advisable to maintain a unit set consistent with the input data (e.g., in terms of solar masses, parsecs, and parsecs/Myr) for Galpy as well, thereby eliminating the need for additional unit conversions. This approach is the default choice.
It is important to note that this differs from the official unit of Galpy, which is based on the solar motion. In the official Galpy unit system, the length unit corresponds to the distance from the Sun to the Galactic center, and the velocity unit represents the solar velocity in the Galactic frame. Therefore, when interpreting suggested argument values of potentials from Galpy, users should calculate these values in PeTar units instead, ensuring consistency across the calculations.
Below is a table illustrating the corresponding units for various output files, with "data" as the example data filename prefix:
| Filename | Content | Unit Set |
|---|---|---|
petar output log |
Printed information from petar |
PeTar unit |
| data.[index] | Snapshots | Particle class: PeTar unit + Stellar evolution unit (refer to petar -h) |
| data.esc.[MPI rank] | Escapers | Time: PeTar unit; Particle: Particle class |
| data.group.[MPI rank] | Multiple systems | Binary parameters: PeTar unit; Particle members: Particle class |
| data.[bse_name].[MPI rank] | Binary stellar evolution events | Stellar evolution unit |
| data.[sse_name].[MPI rank] | Single stellar evolution events | Stellar evolution unit |
| data.status | Global parameters | PeTar unit |
| data.prof.rank.[MPI rank] | Performance profiling | Time: Second (per tree time step) |
In the context of the 'particle class', it denotes the data structure of a single particle (C++ class) within PeTar. Depending on the stellar evolution mode, each particle contains a mix of data from the PeTar component and the stellar evolution component, which may not be in the same unit system. The units for stellar evolution parameters prefixed with "s_" in the particle class can be accessed using petar -h. Other members adhere to the units specified in the input data file (PeTar unit).
Should users require clarification on the units of the output files, they can also refer to the help information provided by the Python analysis tool (help(petar.Particle)) for guidance on interpreting the respective files.
During a simulation, users may encounter warning and error messages in the printed information of petar. When such instances arise, a dump file is generated simultaneously to capture the initial conditions for reproducing the detailed issue. The following section provides an overview of these warnings and errors for user reference.
In scenarios involving a particle cluster with short-range interaction (utilizing Hermite+SDAR), if the relative energy error exceeds the threshold specified by the --energy-err-hard option of petar (default value: 0.0001) during one tree time step, a warning message titled "Hard energy significant" is triggered, and a corresponding dump file named "hard_large_energy.*" is created.
This issue commonly arises when a triple or quadruple system exists within the particle system. The large error can be attributed to two main possibilities:
Resolving these cases without compromising computational efficiency can be challenging. However, if users are concerned about specific particles within the cluster, they can assess the integration orbit's acceptability by employing the debugging tool petar.hard.debug to analyze the dumped "hard_large_energy.*" file. Typically, the high energy error stems from minor changes in the semi-major axis of the tightest binary in the system. Nonetheless, such minor discrepancies typically do not significantly impact the overall dynamical evolution of the system if the error occurs sporadically.
At times, the code's performance may significantly deteriorate, accompanied by a warning indicating large steps. Subsequently, a file named "dump_large_step.*" is generated. This situation typically arises when a stable multiple system exists within the particle cluster.
The AR method is employed to integrate the multiple system, but the step count becomes excessively large, surpassing the predefined step limit (which can be adjusted in the input option), leading to a notable decline in performance. Unfortunately, this scenario is unavoidable in some instances.
Enabling stellar evolution can offer some assistance, especially when the inner binaries are sufficiently tight to merge. However, there is no definitive solution to address this issue. If multiple CPU cores are utilized, users have the option to restart the simulations with fewer CPU cores. Sometimes, upon restarting, the same stable system may not form, thereby circumventing the problem.
Should the stable system persist even after restarting, terminating parallel computing can be considered to eliminate the need for multiple CPUs. Users can temporarily reduce CPU resources to navigate through this phase until the system is disrupted. Subsequently, they can restart with the original number of CPU cores.
When errors manifest during the Hermite-SDAR integration, an error message is displayed, and the simulation is halted, triggering the creation of a file named "hard_dump.*". This occurrence typically signifies the presence of a bug within the code.
Users encountering this issue are encouraged to report it by contacting the developer either through GitHub or email. In the report, users should provide essential details such as the version of PeTar, the configuration options, the initial simulation conditions, and include the "hard_dump.*" file and the input parameter files (prefixed with "input.par.*").
For those inclined to investigate the issue independently, the debug tool petar.hard.debug in conjunction with the GDB tool can be utilized. However, a comprehension of the source codes of SDAR is necessary to interpret the messages generated by the debug tool effectively.
The aforementioned warnings and errors generate dump files that can be analyzed using the petar.hard.debug tool. This tool facilitates the re-execution of the simulation for one tree time step specifically for the isolated hard sub-cluster associated with the warning, aiding in pinpointing the source of the warning or error.
The basic usage of the tool is as follows:
petar.hard.debug [dump_file_name] > debug.log Here, [dump_file_name] refers to the name of the dump files discussed in earlier sections, such as "hard_large_energy.*" and "dump_large_step.*". By executing the command above, the petar.hard.debug tool will display snapshots of particle data per line in the primary output file (debug.log) along with additional information in the printed messages.
To interpret the debug.log file, users can utilize the Python analysis tool petar.HardData. Below is a sample script that reads the debug.log file, converts the first two particles into a binary system, and plots the evolution of the semi-major axis:
# Read petar.hard.debug log, where N_particle represents the total particle number in the sub-cluster (n_ptcl) and N_sd denotes the group number (n_group). Obtain these values from the petar.hard.debug output message.
# Ensure correct option arguments for interrupt_mode and external_mode to accurately interpret the debug.log file.
hard = petar.HardData(member_type=petar.Particle, particle_type='hard', interrupt_mode='bse', external_mode='galpy', N_particle=4, N_sd=2)
hard.loadtxt(path+'debug.log', skiprows=1)
# Retrieve column indices and names
hard.getColumnInfo()
# Convert the first two particles into a binary system
b = petar.Binary(hard.particles.p0, hard.particles.p1, G=petar.G_MSUN_PC_MYR)
# Plot time versus semi-major axis
import matplotlib.pyplot as plt
%matplotlib inline
fig, axes = plt.subplots()
axes.plot(hard.time, b.semi)The initial message in the printed output displays the simulation's input parameters, followed by the particle count (n_ptcl) and group count (n_group). Subsequent messages provide insights into the formation, exchange, and disruption of groups (e.g., binaries, triples). If stellar evolution is active, interruption events are also indicated. These details are instrumental in comprehending the factors contributing to energy errors, the presence of large steps, and pinpointing error locations.
There is one drawback of the current version of petar.hard.debug. When all particles are within a single group, the integration is performed using the pure SDAR method. In this scenario, the debug.log file may remain empty as snapshot files are only generated when the Hermite integrator is utilized.
petar.hard.debug proves more beneficial when used in conjunction with compiler debugging tools like the gdb tool. With gdb, it becomes feasible to track the simulation's progress step by step within the source code to investigate instances of significant energy errors, a high number of steps, or unexpected crashes. To employ gdb, the basic procedure is as follows:
gdb petar.hard.debugSubsequently, in gdb mode, execute:
run [dump_file_name] > debug.logThis command will run petar.hard.debug with the specified dump file name and store the output in debug.log. Users can establish breakpoints in the source code to halt the execution at precise locations and inspect variable values in the vicinity of the source code. This capability proves invaluable for understanding the exact behavior of the petar code and diagnosing issues as they arise. For a more comprehensive understanding, users should familiarize themselves with the usage of gdb beforehand.
At times, the code may crash accompanied by an assertion error message. One common assertion error encountered is n_jp<=pg.NJMAX, as illustrated below:
CalcForceEpEpWithLinearCutoffSimd::operator()(const EPISoft*, ParticleSimulator::S32, const EPJSoft*, ParticleSimulator::S32, ForceSoft*): Assertion `n_jp<=pg.NJMAX' failed.This error typically occurs when the particle system exhibits an extremely high density contrast, or when the density center is distant from the coordinate origin (zero point), or if a particle is significantly far from the system.
The outermost box size during particle-tree construction is determined by the farthest particles in the system. If the maximum box size is excessively large, it results in a large minimum tree cell size, leading to a situation where too many particles may reside in a single cell, surpassing the limits of the particle-tree algorithm and triggering the assertion n_jp<=pg.NJMAX. Additionally, the tree cell closest to the coordinate origin point boasts the highest resolution, hence a distant density center from the origin can also trigger this assertion. Therefore, the resolution lies in removing distant particles or appropriately selecting the coordinate origin point.
Another frequent assertion error is !std::isnan(vbk.x), exemplified by:
SystemHard::driveForOneClusterOMP(ParticleSimulator::F64): Assertion `!std::isnan(vbk.x)' failed.This error is observed when FDPS version 7.1 is utilized. It appears that a bug or an inconsistent interface in FDPS can lead to such assertions within petar. The recommended solution is to revert to using FDPS version 7.0 to mitigate this issue.
Over time, the data formats of snapshots, input parameter files, and certain output files have undergone revisions. Users seeking to utilize a newer version of the code to interpret data from older versions can facilitate data transfer.
For snapshot data in ASCII format, a notable change occurred after the version released on Aug 8, 2020. Specifically, the output format of group_data.artificial transitioned from 64-bit floating point to 64-bit integer to preserve complete information. This alteration solely affects the ASCII format, while the BINARY format remains unchanged. To read older snapshot data, a data conversion step is necessary:
petar.format.transfer -g [other options] [snapshot path list filename]This process generates new data in BINARY format. By employing the same tool with the -b option, users can convert the BINARY format back to the updated ASCII format.
The formats of input parameter files produced during simulations (including files from SSE/BSE and Galpy) were updated on Oct 18, 2020. To adapt the input files for use with newer versions of PeTar, users can employ petar.update.par. Post-update, the reading and modification of input parameter files are significantly improved, enhancing the ease of restarting simulations with the latest PeTar versions.
Several handy tools are available to aid users in generating initial input data, determining an appropriate tree time step to commence simulations, and conducting data analysis. These tools are bundled with petar and follow a naming convention of petar.[tool name]. To access guidance on utilizing each tool, users can employ the following command:
petar.[tool name] -hIt is important to note that options with identical names may hold distinct meanings across various tools.
The subsequent sections provide detailed descriptions of each tool.
PeTar features an internal Plummer model generator for an equal-mass system, utilizing the Henon Unit with a half-mass radius of 1.0. Should users prefer to employ their own initial particle data, the petar.init tool facilitates the conversion of their particle data into a petar input data file. The usage is as follows:
petar.init [options] [particle data filename]The particle data file should consist of 7 columns: mass, position (3 coordinates), velocity (3 components), with each particle represented in a separate row. Binaries should be listed first, with the two components adjacent to each other. When binaries are present, the -b [binary number] option must be included in the petar command to ensure accurate initialization of velocity dispersion, tree time step, and changeover radii.
If stellar evolution is activated, the corresponding options -s [bse_name] should be used concurrently to generate the correct initial files. In such cases, it is recommended to utilize astronomical units (Solar mass [Msun], parsec [pc], and Million years [Myr]) for the initial data. The velocity unit should be specified as pc/Myr, ensuring a mass scaling factor of 1.0 between PeTar units and SSE/BSE-based code. Additionally, the -u 1 option should be added to the petar command to adopt this astronomical unit set.
Similarly, when external mode (potential) is enabled, the -t option should be utilized to ensure the correct number of columns is generated.
The performance of petar is highly dependent on the tree time step chosen. To assist in finding the optimal time step for achieving the best performance, petar.find.dt can be utilized. The usage is as follows:
petar.find.dt [options] [petar snapshot filename]The performance of petar relies on the initial particle data file in the petar input format. This tool conducts brief simulations with various tree time steps and presents the performance results sequentially. Users can then determine which time step yields the best performance.
It is important to note that if a time step that is too large is tested, the tool may not respond for an extended period, indicating a suboptimal choice of time step. In such cases, the tool will terminate the test and provide the best result from the previous trials.
Several options are available in this tool to adjust the numbers of OpenMP threads and MPI processors, as well as the minimum tree time step to initiate the test. If other options are used in the petar command, such as -b [binary number], -u [unit set], or -G [gravitational constant], these options should be included using the -a option with the content enclosed in double quotes:
petar.find.dt [options] -a "[petar options]" [petar data filename]For example:
petar.find.dt -m 2 -o 4 -a "-b 100 -u 1" inputThis command uses 2 MPI processes, 4 OpenMP threads per MPI process, 100 primordial binaries, and a unit set of 1 [Msun, pc, Myr] to determine the best time step.
It is worth noting that petar only accepts tree time steps that are integer powers of 0.5. Therefore, during testing, if the user specifies the minimum step size using -s [value] (outside -a), the step size will be adjusted to meet this requirement if necessary. Users should be cautious as some petar options, such as -o and -s, cannot be used within the -a option of petar.init. Further details can be obtained by using petar.find.dt -h.
For users looking to restart a simulation and automatically determine the new tree time step along with other parameters (radii), the following command can be used:
petar.find.dt -m 2 -o 4 -a "-p input.par -r 0 --r-search-min 0 --r-bin 0" [restart snapshot filename]In MPI usage, each MPI processor generates individual data files with filenames containing the suffix [MPI rank]. To consolidate these output files from different MPI ranks into a single file, the petar.data.gether tool is utilized. Additionally, this tool can split the stellar evolution event files and group files into individual components, enabling the use of Python tools for data analysis (refer to Output files).
Moreover, petar.data.gether generates a file named "[output prefix].snap.lst" that includes a sorted list of all snapshot files based on their respective timestamps. This file serves as input for both petar.data.process and petar.movie.
The basic usage of petar.data.gether is as follows:
petar.data.gether [options] [data filename prefix]Here, [data filename prefix] represents the prefix of data files specified by the petar option -f (default is 'data').
Several options can control the gathered data; use petar.data.gether -h to review the details of [options].
-f: specifies the filename prefix of the gathered data, defaulting to the same as [data filename prefix].-i: prompts whether to overwrite existing gathered data from previous runs of petar.data.gether; if not provided, old files are replaced.-l: generates only the snapshot file list.-g: gathers group files and splits them into separate files based on the number of members in a group.Below is a table detailing the files generated by the tool and the corresponding Python analysis classes for reading (refer to Data analysis in Python3):
| Original files | Output files | Content | Python classes initialization for reading |
|---|---|---|---|
| data.group.[MPI rank] | data.group | all groups | None |
| data.group.n2 | binaries, hyperbolic systems | petar.GroupInfo(N=2) | |
| data.group.n3 | triples | petar.GroupInfo(N=3) | |
| ... | multiple systems... | ... | |
| data.esc.[MPI_rank] | data.esc | escapers | petar.SingleEscaper(interrupt_mode=[*], external_mode=[*]) |
| data.[sse_name].[MPI rank] | data.[sse_name] | full single stellar evolution records | None |
| data.[sse_name].type_change | single stellar evolution type change events | petar.SSETypeChange() | |
| data.[sse_name].sn_kick | supernova natal kick of single star | petar.SSESNKick() | |
| data.[bse_name].[MPI rank] | data.[bse_name] | full binary stellar evolution records | None |
| data.[bse_name].type_change | binary stellar evolution type change events | petar.BSETypeChange() | |
| data.[bse_name].sn_kick | supernova natal kick in binaries | petar.BSESNKick() | |
| data.[bse_name].dynamic_merge | dynamical-driven (hyperbolic) mergers | petar.BSEDynamicMerge(less_output=[*]) |
Here, [*] represents arguments that depend on the configuration options used for compilation.
Note: 'data.group[.n*]' files are not generated by default due to their large size. To obtain these files, the -g option must be added.
When SSE/BSE is employed and the code version is before Sep 10, 2020, data with the suffix ".dynamic_merge" contains three fewer columns compared to the new version. This tool automatically fills the missing columns with zeros from Column 6 to 8.
The petar.data.process tool is utilized for analyzing snapshot data, identifying binaries, triples, and quadruples (specifically binary-binary types), and computing Lagrangian radii, core radii, averaged mass, and velocity dispersion. It is important to highlight that the tool calculates the core (density) center and uses it to determine Lagrangian radii. Single and binary data are saved for each snapshot with the additional suffix ".single" and ".binary", respectively. Triples and quadruples are optional and not used in the computation of Lagrangian properties. Data for Lagrangian, core, and escapers is generated in separate files. Multiple CPU cores are utilized for data processing due to the slow nature of the KDTree neighbor search required for density calculation and binary detection.
The basic usage is as follows:
petar.data.process [options] [snapshot path list filename]Users need to provide [snapshot path list filename] for a file containing a list of paths for the snapshot data files. This file can be generated using the petar.data.gether tool. Alternatively, users can manually create the file using commands like ls and egrep in Linux. For instance, if the snapshot filename prefix is 'data', the command would be:
ls | egrep '^data.[0-9]+$'It is recommended to sort the paths in increasing order of evolution time. The sort tool can be used for this purpose, as shown in the example below:
ls | egrep '^data.[0-9]+$' | sort -n -k 1.6 > snap.lstThis command finds all data files in the current directory, sorts them based on the suffix (values after 'data.') in increasing order, and saves the list to the file 'snap.lst'. The -n flag specifies that the values to sort are floating-point numbers, and -k defines the starting position of the number for sorting.
Users should ensure to set the correct options for gravitational constant (-G), interrupt mode (-i), and external mode (-t) for petar.data.process. This is crucial for reading snapshots and calculating Kepler orbital parameters of binaries. For simulations using astronomical units (-u 1 in the petar command), the gravitational constant -G 0.00449830997959438 should be used for petar.data.process. If using a package like SSE/BSE, the interrupt mode option -i [bse_name] can set the correct value of G. When an external mode like Galpy is employed, the external mode option -t galpy is necessary.
Below is a table showing the files generated by petar.data.process and the corresponding Python modules (classes) for reading them. The default filename prefix 'data' is assumed.
| Filename | Content | Python analysis classes for reading data files |
|---|---|---|
| data.[*].single | snapshots for single stars | petar.Particle(interrupt_mode=[*], external_mode=[*]) |
| data.[*].binary | snapshots for binaries | petar.Binary(member_particle_type=petar.Particle, simple_mode=[*], G=[*], interrupt_mode=[*], external_mode=[*]) |
| *data.[*].triple | snapshots for triples (if option -M is used) |
petar.Binary(member_particle_type_one=petar.Particle, member_particle_type_two=[petar.Particle, petar.Particle], simple_mode=[*], G=[*], interrupt_mode=[*], external_mode=[*]) |
| *data.[*].quadruple | snapshots for binary-binary quadruples (if option -M is used) |
petar.Binary(member_particle_type=[petar.Particle, petar.Particle], simple_mode=[*], G=[*], interrupt_mode=[*], external_mode=[*]) |
| data.lagr | Lagrangian and core properties for all objects, singles, binaries, and user-defined stellar types (add_star_type) |
petar.LagrangianMultiple(mass_fraction=[*], calc_energy=[*], external_mode=[*], add_star_type=[*]) |
| data.core | core position, velocity, and radius | petar.Core() |
| data.esc_single | Single escapers | petar.SingleEscaper(interrupt_mode=[*], external_mode=[*]) |
| data.esc_binary | Binary escapers | petar.BinaryEscaper(member_particle_type=petar.Particle, simple_mode=[*], G=[*], interrupt_mode=[*], external_mode=[*]) |
| *data.bse_status | Evolution of number counts, maximum and averaged masses of different stellar types | petar.BSEStatus() |
| *data.tidal | Tidal radius data (if option --r-escape tidal is used) |
petar.Tidal() |
Note: The arguments [*] for the keywords in the Python class initialization depend on the configure options for compiling (e.g., interrupt_mode, external_mode) and the options used in petar.data.process. These keyword arguments are optional and only needed when default values are not used. Refer to the help of the Python analysis classes and petar.data.process -h for more details.
For details on how to use the Python analysis classes to read data, refer to Data analysis in Python3.
The snapshots generated by petar.data.process are shifted to the rest frame where the density center is the coordinate origin. By adding the core position and velocity from 'data.core' at the corresponding time, positions and velocities in the initial frame or Galactocentric frame (when Galpy is used) can be recovered.
When snapshot files are in BINARY format, the option -s binary can be used for petar.data.process to read the snapshots correctly. It's important to note that the data generated by petar.data.process are all in ASCII format.
Additionally, the petar code can remove escapers and store the data of escapers using energy and distance criteria (in files [data filename prefix].esc.[MPI rank], see Output files). All escapers during the simulations are not stored in the original snapshot files. The petar code only applies a simple constant escape radial criterion. The post-processing by petar.data.process can calculate the tidal radius and detect escapers, which are then stored in the post-generated escape files: "data.esc_single" and "data.esc_binary". These escapers are not removed from the post-generated snapshot files: data.[index].single and data.[index].binary.
For Lagrangian properties, 'data.lagr' includes radius, average mass, number of objects, different components of velocity, and dispersions within different Lagrangian radii. The mass fractions of Lagrangian radii are 0.1, 0.3, 0.5, 0.7, and 0.9 by default. The core radius property is added at the end. There is an option in petar.data.process to define an arbitrary set of mass functions. When using the SSE/BSE-based stellar evolution package, an additional option --add-star-type can be used to calculate Lagrangian properties for specific types of stars. When --add-star-type is used, the reading function should have consistent keyword arguments. An example of reading 'data.lagr' is provided in Reading Lagrangian data.
When --calc-energy is used, potential energy, external potential energy, and virial ratio for each Lagrangian radii are calculated. However, when an external potential is used, the virial ratio may not be accurately estimated in disrupted phases.
The petar.get.object.snap tool enables the collection of specified objects from a list of snapshots into a single file with a time series. Users can define IDs, stellar types, mass ranges, and a custom Python script to select objects.
For instance, if users wish to extract the trajectories of objects with IDs 1 and 2, this tool can scan all provided snapshots and consolidate the data of these objects into a single file. The following script demonstrates this process:
petar.get.object.snap -m id 1_2 [snapshot path list filename]Subsequently, a new file named "object.1_2" is created for objects with IDs 1 and 2. By utilizing petar.Particle from the data analysis module, users can access this file and analyze the evolution of these two objects throughout the simulation. For more information, refer to
the help information of petar.get.object.snap -h.
Similar to configuring petar.data.process, users should ensure the correct settings for interrupt mode (-i), external mode (-t), and snapshot file format (-s) are in place while using petar.get.object.snap. This guarantees the accurate interpretation of the snapshots.
The petar.movie tool is a convenient utility for creating movies from snapshot files. It can generate movies showcasing the positions (x, y) of stars, the HR diagram if stellar evolution (SSE/BSE) is enabled, and the 2D distribution of semi-major axis and eccentricity of binaries. To generate a movie, a list of snapshot files is required.
The basic usage of petar.movie is as follows:
petar.movie [options] [snapshot path list filename]For plotting binary information, it is recommended to first utilize petar.data.process to detect binaries using multiple CPU cores. This preprocessing step eliminates the need for the movie generator to employ the expensive KDTree function for binary detection (use the option '--generate-binary 2').
This tool utilizes either the imageio or matplotlib.animation Python modules to create movies. Installing imageio is advised for faster movie generation using multiple CPU cores, as matplotlib.animation can only utilize a single CPU core. Additionally, it is recommended to install the ffmpeg library to support various commonly used movie formats such as mp4 and avi. Please note that ffmpeg is a standalone library and not a Python module. Users should install it in the operating system (e.g., via the apt tool in Ubuntu).
Similar to configuring petar.data.process, users should ensure to set the correct options for the gravitational constant (-G), interrupt mode (-i), external mode (-t) and snapshot file format (-s) when using petar.movie. This ensures to correctly reading the snapshots.
The petar.data.clear tool serves the purpose of removing data recorded after a specified time from all output files except the snapshots. This tool is particularly useful for preventing the repetition of events when restarting an abnormally interrupted simulation.
In scenarios where a simulation does not terminate normally, the last output snapshot lags behind other output files that record events, such as '*.groups' and '*.bse' files. Consequently, restarting the simulation from this snapshot may lead to the re-recording of the same event in these files.
The basic syntax for utilizing this tool is as follows:
petar.data.clear -t [time] [data filename prefix]Before data removal takes place, all output files undergo a backup process by renaming them with an additional '.bk' suffix. This ensures that, in the event of accidental tool usage, the original files can be restored from the backups.
If the tool is executed again, it automatically checks for the presence of backup data files and utilizes them to create new files with removed data. Essentially, this process is akin to restoring the original file before executing the data removal.
Please be aware that the backup files only retain the data prior to the most recent modification. If the tool is utilized multiple times and the backup files are overwritten, it is important to note that the original data may not be completely recoverable.
Petar offers the capability to read and write snapshot files in either BINARY or ASCII format. The BINARY format, being compressed (resulting in file sizes less than half of the ASCII format), facilitates faster read and write operations for both Petar and data analysis tools. However, it is important to note that BINARY files cannot be directly interpreted using a text editor. It is recommended to opt for the BINARY format when simulations yield a substantial amount of data and users intend to utilize analysis tools for data interpretation. The Petar.Particle and Petar.PeTarDataHeader classes in the Python3 analysis module support reading both BINARY and ASCII formats.
Moreover, it is feasible to convert snapshot data between BINARY and ASCII formats using the petar.format.transfer and petar.format.transfer.post tools.
petar.format.transfer is used for snapshot files outputted from petar. The basic syntax for converting a list of snapshot files is as follows:
petar.format.transfer [options] [snapshot path list filename]The snapshot path list contains paths to the snapshots that users wish to convert. By default, new files are generated with a '.B' or '.A' suffix. To overwrite files for space conservation, users can utilize the -r option. This tool can also update older versions of snapshots in ASCII format (prior to Aug 8, 2020) to newer versions using the -g option. It is important to note that in the older version, certain information stored in the group_data (group center-of-mass mass and velocities in 64-bit floating point) is lost. However, this loss is inconsequential as the data can be recalculated during data processing and does not impact restart operations.
It is essential to ensure that the versions of petar.format.transfer and Petar align in terms of interrupt mode and external mode configurations. In cases where snapshots are generated by different versions of Petar, petar.format.transfer may fail to read data or provide incorrect transferred data.
petar.format.transfer.post is designed for snapshots generated by petar.data.process. The fundamental syntax is as follows:
petar.format.transfer.post [options] [snapshot path list filename]The snapshot path list contains paths to the snapshots that users intend to convert. These snapshots include single, binary, triple, and quadruple snapshots generated from petar.data.process. Users have the flexibility to convert among three formats: ASCII, BINARY, and npy. The npy format corresponds to the Python Numpy data format. It is necessary for users to maintain consistent interrupt mode and external mode settings to ensure successful format conversion.
The formats of input parameter files generated during simulations, including files from SSE/BSE and Galpy, were revised on Oct 18, 2020. To utilize the new version of PeTar for restarting simulations using old versions of input parameter files, an update is required:
petar.update.par [options] [input parameter filename]By employing options such as -p, -b, and -t, users can update input parameters from PeTar, SSE/BSE, and Galpy, respectively. Additional options cater to different features selected in the configuration.
Post-update, the new input parameter files are more user-friendly. They consist of three columns defined as (1) the data type of the argument, (2) option names, and (3) argument values. The reference for the first two columns can be accessed using the command petar -h. Users can directly modify the argument values in the file. Furthermore, it is not necessary to list all options in the file. Consequently, if new options are introduced in future versions, there is no necessity to update the file again unless existing option names undergo changes.
The petar.[bse_name] tool is generated when utilizing the SSE/BSE based stellar evolution package (--with-interrupt=[bse_name]) during configuration, where [bse_name] can be 'bse', 'bseEmp' and 'mobse'. This tool functions as a standalone application for evolving stars and binaries up to a specified time. All essential global parameters can be configured through options.
To evolve a group of stars using the tool:
petar.[bse_name] [options] mass1, mass2 ...If individual masses are not provided, the tool can evolve a group of stars with equal logarithmic mass intervals.
For evolving a group of binaries:
petar.[bse_name] [options] -b [binary data file]In this scenario, the binary data file contains 4 values (mass1, mass2, period, eccentricity) per line. The first line specifically includes the number of binaries. The units of mass and period are contingent on the '--mscale' and '--tscale' options. By default, the units are set to Msun and Myr. For instance, if the tscale is not 1.0, the period in Myr is calculated as the input period value multiplied by tscale.
When there is only one star or one binary, the command line displays the evolution history, including type changes and supernova events. However, if there are multiple stars or binaries, only the final status is printed.
Additional files that document the evolution history of all stars or binaries can be generated by using the -o option. The argument for this option specifies the filename prefix. For instance, when -o output is employed:
Reading these files follows the same method as for the output files from petar (refer to Data analysis in Python3 and Gathering Output Files).
When the external potential package Galpy is compiled with --with-external=galpy during configuration, both petar.galpy and petar.galpy.help are compiled simultaneously.
petar.galpy functions as a standalone tool for computing accelerations and potentials for a particle list using a specified potential model. The basic usage is:
petar.galpy [options] [particle data filename]This tool can create mesh points to measure potential and aid in drawing potential contours for a given potential set.
In the petar command line interface for utilizing Galpy, three options are employed to configure potential models: --galpy-set, --galpy-type-arg, and --galpy-conf-file. The latter two options necessitate users to define potential indices and corresponding arguments. petar.galpy.help provides essential information to assist users in setting up these parameters.
To begin, execute the following command:
petar.galpy.helpThis tool will assist users in generating a configuration file and provide a list of potentials with mathematical formulas, indices, and arguments. These potentials have been tested and verified to function correctly within petar.
Moreover, petar.galpy.help offers a comprehensive list of potentials sourced from the official Galpy documentation. This list includes indices and default arguments, although they have not been extensively tested within petar.
It is crucial to acknowledge that the official Galpy documentation is primarily designed for the Python interface, and certain descriptions may not align perfectly with the C interface. Users may need to consult the Galpy C interface source codes to ensure the proper setup of potential arguments.
For detailed insights into a specific potential, users can utilize:
petar.galpy.help [potential name]This command fetches the potential definition from the official Galpy documentation (note: not extensively tested). Additionally, the -o option enables the creation of a configuration file template of a specific potential. After adjustment of this file, it can be read by the petar command line option: --galpy-conf-file.
It is essential to include the relevant references when publishing results obtained using PeTar. These references can be found in the help function of petar and are displayed at the start of the output following a simulation run. Additionally, when activating a feature imported from an external library such as SSE/BSE or Galpy, the corresponding references are automatically included in the output.
The help information provides a comprehensive list of all available options and can be accessed using the '-h' option for petar and its associated tools. For instance:
petar -h
petar.data.process -hThese commands offer detailed descriptions of the input particle data file format and available options. It is recommended to review the help information prior to utilizing petar and its tools to mitigate errors. Updates corresponding to new PeTar versions are consistently integrated into the help information, keeping users informed about the latest features and functionalities.
PeTar features a Python module designed for data analysis purposes. This module facilitates the reading and analysis of output files generated by petar and its tools, identification of multiple systems, calculation of Lagrangian radii and core radii, analysis of system energy errors, and performance evaluation of different parts of the code.
To utilize this module, start by importing it in a Python script, IPython, or Jupyter notebook:
import petarEnsure that after installing PeTar, the include directory of PeTar has been added to the PYTHONPATH environment variable to successfully import this module.
The module is structured using Python classes and functions. Each class is responsible for reading a specific output file, while functions are utilized for data analysis tasks.
After reading a file using a specific class, users can access the class members for analysis, such as mathematical calculations, data selection, and plotting data. Each class member represents a physical parameter, and its data type can be either a NumPy array or another class as a subclass. The array can be 1D or 2D, storing single or multiple columns from the output file, respectively. The first dimension of the array corresponds to the row index in the data file.
For instance, the petar.Particle class is used for reading snapshot files outputted by petar during a simulation. This class includes members like mass, represented as a 1D NumPy array where each element records the mass of a particle. The array size is equal to the total number of particles ($N$).
The class also contains a member pos, a $N\times3$ 2D NumPy array where the first dimension represents the number of particles, and the second dimension represents the position vector of each particle.
If the SSE/BSE is activated, the class includes a member star, a subclass of type petar.SSEStarParameter that stores the stellar evolution parameters of particles.
All classes have special members like size, ncols, keys, and host. These members signify:
size: the data size, equivalent to the size of a 1D array member.ncols: the total number of columns read from the output files, summing column counts of all data members. For a 2D array member like pos of $N\times3$, it counts as 3. If a member is a subclass, it counts the ncols value of that subclass.keys: the names and data types of all data membershost: when the class instance is a member of another class instance, such as star in petar.Particle, host references the parent class instance, otherwise it is None.To utilize these classes, users must create a class instance by executing:
[class instance] = petar.[class name]([keyword arguments])Here, [class instance] represents the name of a class instance, and [class name] represents the class name, e.g., petar.Particle.
After creating the class instance, users can employ [class instance].keys or [class instance].getColumnInfo() to view the actual list of members. The latter function also provide the corresponding column index in the output file for each member.
Using help([class name]) or help([variable name]) reveals the names, types, definitions of class members (keys) and the available keyword arguments. For description of members, the type "1D" or "2D" indicates a NumPy array member. Otherwise, it denotes the subclass type name, and the corresponding member is its class instance containing a subset of data (multiple columns in data files). Users can further explore member definitions in the subset of data by using help([class instance].[member name]). The description of the __init__ method in the help information provide the available keyword arguments.
In certain classes, the list of members may vary depending on the keyword arguments used to create the instance. petar.Particle exemplifies this scenario. The help information of this class categorizes members into groups, and the final member list is a combination based on the keyword arguments used.
The table below lists all class names (omit the prefix "petar."), corresponding keyword arguments, and output files. For convenience, the output file prefix used in the following filenames is 'data'.
petar (requires using petar.data.gether):| Class name | Description | Keyword Arguments (options shown in []) | Corresponding file |
|---|---|---|---|
| PeTarDataHeader | Header (first line) of snapshot data | external potential option: external_mode=['galpy', 'none'] |
data.[index] |
Data format: snapshot_format=['binary', 'ascii'] |
|||
| Particle | Particle data | stellar evolution option: interrupt_mode=['bse', 'mobse', 'bseEmp', 'none'] |
data.[index], data.[index].single |
external potential option: external_mode=['galpy', 'none'] |
|||
| Status | Global parameters (energy, N ...) | data.status | |
| Profile | Performance metrics of code parts | GPU usage: use_gpu=[True, False] |
data.prof.rank.[MPI rank] |
| GroupInfo | Multiple systems (binary, triple ...) | Number of members in systems: N=[2, 3, ...] |
data.group.n[number of members] |
petar or petar.[bse name] with SSE/BSE stellar evolution:| Class name | Description | Corresponding file |
|---|---|---|
| SSETypeChange | Type change records of single stars | data.[sse_name].type_change |
| SSESNKick | Supernove kick events of single stars | data.[sse_name].sn_kick |
| BSETypeChange | Type change records of binary stars | data.[bse_name].type_change |
| BSESNKick | Supernove kick events of binary stars | data.[bse_name].sn_kick |
| BSEDynamicMerge | Dynamically driven mergers | data.[bse_name].dynamic_merge |
| BSEMerge | Mergers of binaries | Generated by using the class function combine to gather information from instances of petar.BSETypeChange and petar.BSEDynamicMerge types. |
| tide | Dynamical tide or hyperbolic gravitational wave events | data.[bse_name].tide |
petar.data.process:| Class name | Description | Keyword arguments | Corresponding file |
|---|---|---|---|
| SingleEscaper | Single star escapers | same as petar.Particle |
data.esc (from petar), data.esc_single |
| BinaryEscaper | Binary star escapers | same as petar.Binary |
data.esc_binary |
| LagrangianMultiple | Lagrangian and core properties | mass_fraction, calc_energy, external_mode, add_star_type, add_mass_range, calc_multi_rc |
data.lagr |
| Core | Core radius, center position and velocity of the system | data.core | |
| Binary | Binary and multiple system | member_particle_type, member_particle_type_one, member_particle_type_two,interrupt_mode, external_mode, simple_mode, G |
data.[index].binary, data.[index].triple, data.[index].quadruple |
| BSEStatus | Stellar evolution statistics: the evolution of number counts, maximum and averaged masses of different stellar types | data.bse_status |
For more information on the keyword arguments, refers to the Parallel data process section for a detailed description of the keyword arguments.
The module also includes several useful functions that can be explored using help(Function name) in Python. The following table summarize the names and functionalities:
| Function name | Description |
|---|---|
| join | Join two data instances of the same type. Example: petar.join(particle1, particle2) creates a new petar.Particle instance with combined data |
| findPair | Detect binaries of from a particle snapshot data using scipy.cKDTree |
| findMultiple | Detect triples and binary-binary quadruples from single and binary data. |
| parallelDataProcessList | Process a list of snapshot files in parallel to generate single and binary snapshots, Lagrangian data, core data and escaper data. This is the main function used in petar.data.process |
| vecDot | Dot product of two 2D arrays |
| vecRot | Rotate a 3D vector array using Euler angles via scipy.spatial.transform.Rotation) |
| cantorPairing | Generate a new ID from two IDs, useful for obtaining unique binary IDs |
| calcTrh | Calculate one-component half-mass relaxation time using Spitzer (1987) formula |
| calcTcr | Calculate half-mass crossing time |
| calcGWMyr | Calculate the merging timescale in Myr for gravitational waves using Peters (1964) formula |
| convergentPointCheck | Calculate proper motions in the frame of the convergent point and determine residuals (van Leeuwen F., 2009; Jerabkova T. et al. 2021) |
| petar.coordinateCorrection | Correct the c.m. coordinate based on the difference between the snapshot center and the observational center in the galactocentric frame |
Additional useful tools will be implemented in the future. The tools/analysis/parallel_data_process.py serves as a good example for learning how to utilize the analysis tool.
The following sections provide exmaples of using the classes to read and analyze output files.
Here is an example of using the petar.Particle class for reading a snapshot of particles. Snapshots generated by petar consist of two parts: a header and data. In ASCII format, the first line is the header, followed by the data of each particle per line.
For example, the first snapshot at time zero generated by petar is named 'data.0' by default. To obtain its header information, the petar.PeTarDataHeader class can be used:
import petar
header = petar.PeTarDataHeader('data.0')If the keyword argument snapshot_format is not specified, the data is assumed to be in ASCII format. To read the BINARY format:
header = petar.PeTarDataHeader('data.0', snapshot_format='binary')After reading, the header contains three members: fid, n, and time, representing the file ID, number of particles, and time (in the same unit as that of the input model) of the snapshot, respectively.
If external_mode=galpy, the header contains additional members: the position and velocity offsets, pos_offset and vel_offset, representing the shift of the system's center in the Galactic tidal field (assuming the coordinate origin is the galactic center).
To read the particle content in ASCII format:
particle = petar.Particle(interrupt_mode='bse')
particle.loadtxt('data.0', skiprows=1)Here, the keyword argument interrupt_mode is crucial for proper snapshot reading. The column definitions in snapshots depend on the stellar evolution option (--with-interrupt) and the external potential option (--with-external) used during configuration. The argument bse indicates that the updated SSE/BSE is used, so external columns exist in the snapshots. In this case, particle contains a member star with the class type petar.SSEStarParameter. Similarly, if an external potential is added, one more column pot_ext is included.
Since the first line in the snapshot file is the header, skiprows=1 is used to skip this line when reading data.
If the snapshot data is in BINARY format, the fromfile function should be used instead of loadtxt:
particle.fromfile('data.0', offset=petar.HEADER_OFFSET)Here, fromfile is similar to numpy.fromfile. The keyword argument dtype is implicitly defined, and users should not change it. The offset keyword sets the byte offset to read the data. petar.HEADER_OFFSET is a constant indicating the snapshot header line offset, equivalent to skiprows=1 in the loadtxt function. If an external potential is included with the corresponding configuration option --with-interrupt=galpy, the offset should be set to petar.HEADER_OFFSET_WITH_CM.
When using the Python analysis tool to read data, users must ensure that the keyword arguments in the initialization function align with the options set in the PeTar configuration during installation and the options in the data analysis tool petar.data.process. This is crucial to prevent incorrect data reading.
For instance, if the configuration includes bse with --with-interrupt=bse, additional columns of stellar evolution parameters are saved in snapshot files. If the initialization of petar.Particle lacks the keyword argument interrupt_mode='bse' like this:
particle = petar.Particle()
particle.loadtxt('data.0', skiprows=1)The particle object will not contain the correct data. In such cases, a warning message will be displayed:
UserWarning: The reading data shape[1] or the number of columns (34) mismatches the number of columns defined in the class instance (20)! Make sure whether this is intended and whether you properly choose the correct keyword arguments for the class instance initializationHere, the snapshot file 'data.0' has 34 columns (excluding the first line) that include the stellar evolution parameters, while particle is set to have only 20 columns (ncols=20). This mismatch can lead to incorrect assignment of data columns and class members. Therefore, when this warning appears, users should review whether they have forgotten or incorrectly set the keyword arguments during initialization.
It's important to note that by default, Python displays the warning only once. If the same part of the code is executed multiple times, the warning may not reappear even if the data reading is incorrect. To always show the warning message, users can execute the following command first:
import warnings
warnings.simplefilter('always')Users can access particle information such as masses via particle.mass. Since particle.mass is a NumPy array, it allows for flexible mathematical operations. For example, to calculate the average mass of all particles, users can use:
import numpy as np
mave = np.average(particle.mass)To compute the center of mass (c.m.) position of particle systems, users can perform the following calculation:
import numpy as np
cm_pos = np.sum(particle.pos * particle.mass[:, None], axis=0) / particle.mass.sum()To retrieve the number of particles (line numbers in snapshots excluding the header):
print(particle.size)Users can utilize NumPy-like indexing, slicing, and conditional selection for PeTar class instances.
For example, to select the data of the first particle:
first_particle = particle[0]To slice the data of the first 10 particles:
particle_set = particle[:10]To apply a filter and create a subset of data with particle masses less than 1.0:
particle_set = particle[particle.mass < 1.0]This operation is akin to the getitem function of a NumPy array.
The indexing, slicing, and selection can also be applied to the members:
pos_set = particle.pos[particle.mass < 1.0]This generates a 2D NumPy array of particle positions with masses below 1.0.
Utilizing the NumPy-style data, users can leverage plotting modules such as Matplotlib to create visualizations with PeTar data.
For instance, to plot the mass-distance relation of the subset data with mass < 1.0 using Matplotlib:
import matplotlib.pyplot as plt
fig, axes = plt.subplots(1, 1)
particle_set = particle[particle.mass < 1.0]
particle_set.calcR2()
axes.plot(np.sqrt(particle_set.r2), particle_set.mass, '.')Users have the option to save the post-processed data to a new file.
For instance, to save the subset data generated in the previous section in ASCII format:
particle_set.savetxt([file path])It's important to note that when additional members are added to the particle instance, the saved data will also include the additional columns. In the given example, particle_set.calcR2() generates a new class member, r2 (distance squared). Therefore, the saved data will have an additional column at the end, which did not exist in the original snapshot. When users read this saved data, they should first add the r2 member to ensure correct column reading:
import numpy as np
particle_new = petar.Particle(interrupt_mode='bse')
particle_new.addNewMember('r2', np.array([]))
particle_new.loadtxt([file path])Users can also save and load data in BINARY format by using tofile instead of savetxt and fromfile instead of loadtxt, respectively:
# save
particle_set.tofile([file path])
# load
particle_new.fromfile([file path])Additionally, users can save and load data in NumPy format:
# save
particle_set.save([file path])
# load
particle_new.load([file path])The petar.Particle and petar.Core classes provide a member function to convert the data type to astropy.coordinates.SkyCoord. SkyCoord is a powerful Python module that facilitates easy transformation of the reference frame and coordinate system of particle data.
For instance, when using Galpy for simulations in petar, the Galactocentric frame with the Cartesian coordinate system is typically employed. In scenarios where no stellar evolution is utilized, the input unit is in astronomical units (Msun, pc, pc/Myr), and the output format is ASCII. Below is a script to transform a single snapshot without stellar evolution and with an ASCII output format:
import petar
import astropy.units as units
# Read snapshot data from petar
particle = petar.Particle(external_mode='galpy')
particle.loadtxt([snapshot path], skiprows=1)
# Read center of mass offset in the Galactocentric frame
header = petar.PeTarDataHeader([snapshot path], external_mode='galpy')
# Obtain SkyCoord data type in the Galactocentric frame
particle_new = particle.toSkyCoord(pos_offset=header.pos_offset, vel_offset=header.vel_offset)This script will generate a new data set particle_new with the type astropy.coordinates.SkyCoord. It's important to note that the solar position (galcen_distance=8.0*units.kpc, z_sun=15.*units.pc) and velocity (galcen_v_sun=CartesianDifferential([10.0, 235., 7.]*u.km/u.s)) assumed in galpy differ from the default values of SkyCoord. The values in the toSkyCoord function align with the galpy assumptions.
Subsequently, plotting the data (RA, DEC) in the ICRS frame using Matplotlib becomes convenient:
import matplotlib.pyplot as plt
fig, axes = plt.subplots(1, 1)
ra = particle_new.icrs.ra
dec = particle_new.icrs.dec
axes.plot(ra, dec, '.')
axes.set_xlabel('RA')
axes.set_ylabel('Dec')To combine two subsets of particle data, particle_set1 and particle_set2, into one, you can use the following command:
particle_merge = petar.join(particle_set1, particle_set2)For instance, if the sizes of the two sets are 3 and 5, respectively, the new instance particle_merge will have a size of 8.
Each class provides a set of useful functions for data management. Below is a table outlining these functions:
| Function Name | Description |
|---|---|
addNewMember(key, member) |
Add a new data member with the name key and content member |
getColumnInfo() |
Retrieve column positions (counting from 0), key member names, and data types from the data file being read |
printTable(column_format, print_title) |
Print a table with specified column list and formats |
append(data) |
Append data to the current class instance |
resize(N) |
Resize the size of the class instance |
loadtxt(file_path) |
Load data in ASCII format from a file |
savetxt(file_path) |
Save data in ASCII format to a file |
load(file_path) |
Load data in NumPy format from a file |
save(file_path) |
Save data in NumPy format to a file |
fromfile(file_path) |
Read data in BINARY format from a file |
tofile(file_path) |
Save data in BINARY format to a file |
In addition to these functions, PeTar classes also support basic mathematical operators such as addition and subtraction. For example, when dealing with two sets of particles, executing the following command will create a new class instance where each member is the sum of the corresponding members in particle_one and particle_two:
particle_add = particle_one + particle_twoIn the preceding sections, we demonstrated how to read and analyze snapshots generated by petar. Here is an additional example illustrating how to read binary snapshot files produced by the petar.findPair function or petar.data.process.
When reading binary data, users need to pay attention to the member particle type. A reliable approach to reading snapshots when SSE/BSE is employed is as follows:
p1 = petar.Particle(interrupt_mode='bse')
p2 = petar.Particle(interrupt_mode='bse')
binary = petar.Binary(p1, p2)
binary.loadtxt([binary data file path])Alternatively, users can specify the member particle type explicitly along with other parameters:
binary = petar.Binary(member_particle_type=petar.Particle, interrupt_mode='bse', G=petar.G_MSUN_PC_MYR)
binary.loadtxt([binary data file path])In the 'bse' mode, the gravitational constant G should be provided in the unit set of Msun, pc, and Myr (0.00449830997959438). Additionally, petar.G_HENON represents the gravitational constant in the Henon unit (equal to 1), which is the default value in petar.Binary.
petar.Binary can also handle triple and quadruple snapshots for reading purposes. To read triple snapshots, you can use the following approach:
binary = petar.Binary(member_particle_type_one=petar.Particle, member_particle_type_two=[petar.Particle, petar.Particle])
binary.loadtxt([triple data file path])In this setup, petar.Binary is structured as a binary tree, with the first component representing the outer single particle and the second component representing the inner binary.
Likewise, for binary-binary quadruple data, the process is as follows:
binary = petar.Binary(member_particle_type=[petar.Particle, petar.Particle])
binary.loadtxt([quadruple data file path])Here, member_particle_type denotes the type (binary) of both components in the quadruple system.
To extract and analyze Lagrangian data generated by petar.data.process, users can follow these steps:
lagr = petar.LagrangianMultiple()
lagr.loadtxt([data.lagr path])The Lagrangian data file contains three subsets: all, single, and binary, representing the Lagrangian data of all objects, single objects, and binaries, respectively. Each member in these subsets is stored as a 2D NumPy array, with properties at various Lagrangian radii and core radii recorded in each row. By default, the mass fraction is set to (0.1, 0.3, 0.5, 0.7, 0.9), resulting in six members in each row, with the final member representing core properties.
For example, to access the half-mass radius and core radius at a mass fraction of 0.5 for all objects:
rh = lagr.all.r[:,2] # half-mass radius
rc = lagr.all.r[:,5] # core radiusSimilarly, to retrieve the average mass at the half-mass radius:
mrh = lagr.all.m[:,2]When utilizing petar.data.process, the -m option allows users to include an arbitrary set of mass fractions. If the SSE/BSE-based stellar evolution package is used, the --add-star-type option in petar.data.process can be used to compute Lagrangian properties for specific types of stars. When employing --add-star-type, additional subsets such as "BH" and "MS" are appended to the Lagrangian data file.
To ensure accurate data retrieval, it is essential to maintain consistency between the options used in petar.data.process and the keyword arguments in LagrangianMultiple. When reading the data, remember to include relevant keyword arguments, such as add_star_type.
For instance, if users want to calculate Lagrangian properties for a subset of black holes and main sequence stars after running a simulation with SSE/BSE and Galpy enabled, the command would be:
petar.data.process -i bse -t galpy --add-star-type BH,MS data.snap.lstSubsequently, in Python to read the data.lagr file generated by petar.data.process:
lagr = petar.LagrangianMultiple(external_mode='galpy', add_star_type=['BH', 'MS'])
lagr.loadtxt([data.lagr path])Inconsistencies in setting the external_mode and add_star_type arguments may lead to warnings or crashes during data loading. One effective method to ensure consistency is by verifying the column numbers in the data file and validating the reading process, as described in Checking Reading Consistency.
Additionally, the --add-mass-range option in petar.data.process can compute Lagrangian properties for a subset of particles with specified mass ranges. For detailed information on --add-star-type and --add-mass-range, refer to petar.data.process -h.
When using SSE/BSE-based stellar evolution packages like updated BSE in a simulation with petar or isolated stellar evolution with petar.bse, files data.bse.* and data.sse.* are generated (assuming the default filename prefix 'data' is used). After executing petar.data.gether data, several new files are created with the suffixes "type_change", "sn_kick", and "dynamic_merge", corresponding to stellar or binary type change, supernova kick and dynamically driven merger events.
To read these files, users can utilize the following command:
path='./'
prefix='data'
sse_type=petar.SSETypeChange()
sse_type.loadtxt(path+prefix+'.sse.type_change')
sse_kick=petar.SSESNKick()
sse_kick.loadtxt(path+prefix+'.sse.sn_kick')
bse_type=petar.BSETypeChange()
bse_type.loadtxt(path+prefix+'.bse.type_change')
bse_kick=petar.BSESNKick()
bse_kick.loadtxt(path+prefix+'.bse.sn_kick')
bse_dyn=petar.BSEDynamicMerge()
bse_dyn.loadtxt(path+prefix+'.bse.dynamic_merge')Here, path denotes the simulation directory path, and prefix represents the filename prefix, which defaults to 'data'.
After reading these files, users can display the events in a table. For instance, to print binary stellar evolution events:
bse_type.printTable([('type','%4d'),('init.time','%10g'),('init.type1','%11d'),('init.type2','%11d'),
('init.m1','%9f'),('init.m2','%9f'),('init.semi','%10g'),('init.ecc','%9f'),
('final.type1','%12d'),('final.type2','%12d'),('final.m1','%9f'),('final.m2','%9f'),
('final.semi','%11g'),('final.ecc','%10g')])In this snippet, printTable is the function used to display selected columns in a table with specified printing formats.
By employing petar.BSEMerge, users can compile potential merger events from BSETypeChange and BSEDynamicMerge:
merger = petar.BSEMerge()
merger.combine(bse_type, bse_dyn)
merger.printTable()It's important to note that the initial status from BSEMerge pertains to the first event record of the binary that undergoes a merger. Furthermore, if a supernova completely removes the material of stars without leaving any remnants, it may be mistakenly identified as a "merger". Users should thoroughly examine the stellar evolution history to exclude such false merger events.
During a simulation, PeTar records information about the formation and dissolution of various systems, including hyperbolic encounters, binaries, triples, quadruples, and more, during SDAR integration. This information is saved into files named "data.group.[MPI rank]", where "data" serves as the default filename prefix. By utilizing petar.data.gether -g [filename prefix], groups with different member counts are separated into individual files named "data.group.n1", "data.group.n2", and so on, with the number indicating the number of members in the multiple systems. The following example illustrates how to read the groups file and analyze the information:
# Load two-body groups (binary, hyperbolic encounters)
g2 = petar.GroupInfo(N=2)
g2.loadtxt(path+'data.group.n2')
# Load 3-body groups
g3 = petar.GroupInfo(N=3)
g3.loadtxt(path+'data.group.n3')
# Load 4-body groups
g4 = petar.GroupInfo(N=4)
g4.loadtxt(path+'data.group.n4')For $N>2$, such as g3 and g4 in the above example, they contain members named bin0, bin1, and so on, indicating pairs of objects assuming a Kepler orbit in a hierarchical order. For instance, bin0 comprises two objects with the greatest separation in the multiple system, and these objects can be either individual particles or the center of mass of the inner systems.
The following example presents a table illustrating the 3-body system, where 'bin0' represents the outer pair and 'bin1' denotes the inner pair. The center of mass of the inner pair is one of the members of the outer pair, with the ID of the center of mass particle being the lower of the two inner member IDs.
g3.printTable([('bin0.m1','%10.4f'),('bin0.m2','%10.4f'),
('bin0.p1.id','%11d'),('bin0.p2.id','%11d'),
('bin0.semi','%10.4g'),('bin0.ecc','%10.4g'),
('bin1.m1','%10.4f'),('bin1.m2','%10.4f'),
('bin1.p1.id','%11d'),('bin1.p2.id','%11d'),
('bin1.semi','%10.4g'),('bin1.ecc','%10.4g')])The previous sections have demonstrated how to read and utilize various petar Python classes. The process for using other classes is quite similar, with the distinction lying in the class members.
To access detailed information about each class and function, Python's help function can be incredibly useful. For instance, to obtain manuals for specific classes like petar.Particle and petar.GroupInfo, you can execute the following commands:
help(petar.Particle)
help(petar.GroupInfo)By utilizing the help function in Python, users can gain insights into the functionalities, methods, and attributes of different classes within the petar package. This approach provides a convenient way to explore the capabilities and usage guidelines of each class, enabling users to make the most of the petar tools effectively.
PeTar offers three methods for conducting collisional N-body simulations. The integration of particle orbits follows a basic cycle, outlined below. For more in-depth information, please refer to the reference paper on PeTar.
Search Clusters and Few-Body Systems
Kick (Soft) Step
Drift (Hard) Step
PeTar employs various parallelization techniques to enhance the efficiency of simulations for large values of $N$. The parallel methods utilized in different components include:
When appropriate tree time steps and changeover radii are set, the performance of hard calculations can be comparable to that of soft force calculations. In such cases, the use of GPUs may not significantly enhance performance, unlike in the direct N-body method for soft forces. Therefore, for optimal performance with large $N$, it is advisable to utilize more CPU cores rather than a few CPU cores with GPUs. This recommendation is particularly relevant when a substantial number of binaries are present in the simulation.
By leveraging these parallelization methods effectively, PeTar can efficiently handle the computational demands of large-scale N-body simulations, ensuring robust and accelerated performance across various simulation scenarios.
AMUSE stands as a robust software suite that amalgamates various codes, ranging from hydrodynamic and N-body simulations to stellar evolution and radiation transfer models.
Presently, PeTar has been integrated as a module within AMUSE, offering support for gravitational dynamics and gravity field computations. This integration enables users to couple PeTar with hydrodynamic codes, facilitating simulations of collisional stellar systems immersed in gas environments.
It is important to note that the stopping condition feature is currently under development and not yet operational. As a result, the merging of binaries and rapid stellar evolution events like supernova kicks are not supported at this time.
The integration of PeTar into the AMUSE API opens up new avenues for conducting complex simulations that combine gravitational dynamics with other physical processes, paving the way for comprehensive studies of stellar systems within diverse astrophysical contexts.