Open NirViaje opened 5 years ago
Alan W. Harris and Line Drube German Aerospace Center (DLR) Institute of Planetary Research, Rutherfordstrasse 2, D-12489 Berlin, Germany; alan.harris@dlr.de Received 2014 February 3; accepted 2014 March 8; published 2014 March 24
https://www.researchgate.net/publication/261034084_How_to_find_metal-rich_asteroids
The Near-Earth Asteroid Thermal Model (NEATM; Harris 1998), based on spherical geometry, offers a relatively straightforward means of deriving reasonably accurate diameters and albedos of asteroids and trans-Neptunian objects (in principle all atmosphereless bodies) from thermal-infrared data for objects with unknown physical characteristics. With NEOs in mind, the NEATM was designed to extend the applicability of the thermal model concept described by Lebofsky et al. (1986) to objects with significant thermal inertia and/or rapid rotation. The model incorporates a fitting parameter, η, referred to for historical reasons as the beaming parameter, which allows the model surface temperature distribution to be adjusted to take account of the effects of thermal inertia, spin vector, and surface roughness, thereby giving a better fit of the model fluxes to the measurements.
NEO | Tax. | PHA? | D(km) | pv | η | ηerr | pIR |
---|---|---|---|---|---|---|---|
138359 | N | 1.09 | 0.10 | 2.931 | 0.105 | 0.19 | |
1865 | S | N | 1.61 | 0.14 | 2.902 | 0.036 | 0.27 |
152931 | Q | N | 1.65 | 0.24 | 2.884 | 0.138 | 0.24 |
152978 | S: | Y | 0.53 | 0.11 | 2.641 | 0.116 | 0.19 |
365071 | Y | 0.87 | 0.15 | 2.559 | 0.117 | 0.28 | |
3554 | X, M, D | N | 3.05 | 0.09 | 2.411 | 0.072 | 0.19 |
215442 | N | 0.79 | 0.15 | 2.328 | 0.325 | 0.17 | |
152558 | S | N | 1.36 | 0.18 | 2.284 | 0.051 | 0.28 |
366774 | AS | Y | 0.86 | 0.20 | 2.284 | 0.059 | 0.29 |
250680 | Y | 0.40 | 0.15 | 2.279 | 0.075 | 0.30 | |
7822 | S | Y | 1.21 | 0.13 | 2.261 | 0.049 | 0.30 |
163243 | S, Q | Y | 1.68 | 0.17 | 2.191 | 0.061 | 0.23 |
263976 | L | Y | 0.79 | 0.13 | 2.165 | 0.043 | 0.18 |
142464 | N | 0.89 | 0.12 | 2.139 | 0.044 | 0.22 | |
2002 NW16 | N | 0.85 | 0.16 | 2.118 | 0.066 | 0.26 | |
103067 | S | Y | 1.28 | 0.25 | 2.114 | 0.056 | 0.29 |
363024 | Y | 0.56 | 0.10 | 2.055 | 0.067 | 0.24 | |
325102 | N | 0.36 | 0.12 | 2.048 | 0.063 | 0.18 |
Light Touch2 : Effective Solutions to Asteroid Manipulation, ESA General Studies Programme
Publication: Massimiliano Vasile https://www.google.com.hk/search?q=Vasile+asteroid https://www.youtube.com/watch?v=mOtIwp86rF0 Vasile-solar-deflection Hazardous asteroid mitigation- Campaign planning and credibility analysis, thesis, Yohei Sugimoto, 2014_2014sugimotophd.pdf
Hodges, Richard E. (21 February 2017). "A Deployable High-Gain Antenna Bound for Mars: Developing a New Folded-panel Reflectarray for the First CubeSat Mission to Mars". IEEE Antennas and Propagation Magazine. 59: 39–49. doi:10.1109/MAP.2017.2655561 – via IEEE Xplore Digital Library.
On board the two CubeSats is an ultra-high frequency (UHF) antenna which is circularly polarized. The EDL information from InSight was transmitted through the UHF band at 8 kbit/s to the CubeSats, and was simultaneously retransmitted at an X band frequency at 8 kbit/s to Earth.[18] MarCO used a deployable solar panel for power, but because of the limitations in solar panel efficiency, the power for the X-band frequency can only be about 5 watts.
In order for the CubeSats to be able to relay information, they need to have a high gain antenna (HGA) which is reliable, meets the mass specs, has low complexity, and is affordable to build. A high gain antenna is one that has a focused, narrow radiowave beam width (directional antenna). Three possible types of antennas were assessed: a standard microstrip patch antenna, a reflectarray, and a mesh reflector. With the small, flat, size required for the CubeSats, the reflectarray antenna type met all of the mission needs. The components of a reflectarray HGA are three folded panels, a root hinge which connects the wings to the body of the CubeSat, four wing hinges, and a burn wire release mechanism. The antenna panels must be able to withstand a varying degree of temperature changes throughout the mission as well as vibrations throughout deployment.[18] MarCO relayed EDL-critical data 8 minutes after the completion of the landing.[19][20]
https://en.wikipedia.org/wiki/Mars_Cube_One#Relay
Membrane optics is a flat lens that employs plastic in place of glass to diffract rather than reflect or refract light. Concentric microscopic grooves etched into the plastic provide the diffraction.[1]
Glass transmits light with 90% efficiency, while membrane efficiencies range from 30-55%. Membrane thickness is on the order of that of plastic wrap.[1]
MEMS Mega-pixel Micro-thruster Arrays for Small Satellite Stationkeeping, EPPDyL, 2000
In-Orbit Demonstration of a MEMS-based Micropropulsion System for Cubesats, Sweden and CAS, 2015
[Catalytic Porous Microchannel for Hydrogen Peroxide MEMS Thruster, Koji Takahashi, Kyushu University, 2006](http://www.aero.kyushu-u.ac.jp/aml/MEMS/article4.pdf
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液体密度:3057kg·m⁻³(-108.10℃,101.325kpa) 储罐压力:30MPa
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