Review script for paper "2023A&A...675A..98M" made with predictor "DataLinkerWithSupport"

[abuonomo]

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bibcode: 2023A&A...675A..98M predictor: DataLinkerWithSupport annotated pdf: view here (requires login)

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[abuonomo]

No date input for script causing the python code to not run correctly.

This happens because the instrumentation form did not pull out the overall date. Looks like its October 25 2013.

2. Observations and data analysis 2.1. Radio emission For a type II radio burst identified on 25 October 2013 no CME association could be made despite a good coverage of multiview-point coronagraph observations (Morosan et al. 2021). No co-temporal CMEs were found in either LASCO C2 coronagraphs or the STEREO A and B COR1 and COR2 coronagraphs. The only eruptive signature that occurred during this Type II was the onset of a C2.3-class flare from the active region NOAA 11875 (Fig. 1a). The Type II radio burst was observed in dynamic spectra from the e-CALLISTO network (Benz et al. 2005) and the ORFEES (Observation Radio pour FEDOME et l’Étude des Éruptions Solaires; Hamini et al. 2021) radio spectrograph in the frequency range 50–190 MHz. The burst shows both fundamental and harmonic emission lanes with band-splitting and was preceded by a set of type III bursts (Fig. 1b). Some of the type III bursts did not continue to lower frequencies and show an inverted J-shape (labelled J-bursts in Fig. 1b). These J-bursts represent a sub-type of type III radio bursts where electrons do not escape along open magnetic field lines but instead propagate along closed coronal loops (e.g. Reid & Ratcliffe 2014; Morosan et al. 2017). The type II burst lasts for ∼5 minutes and ends at a frequency of 50 MHz. At lower frequencies, there was no type II emission and only some interplanetary type III bursts were observed at Article number, page 3 of 10 A&A proofs: manuscript no. aanda Fig. 3. Zoomed-in dynamic spectrum of the type II burst and its flux density over time obtained from NRH images. The top panel shows the ORFEES dynamic spectrum during the type II harmonic lane. The last two panels show the flux of the type II bands together with the relative intensity extracted from the ORFEES dynamic spectrum at two frequencies: 173 (middle) and 150 MHz (bottom). These plots show that the radio sources imaged by the NRH represent the type II emission seen in the ORFEES dynamic spectrum. the time. The harmonic lane of the type II burst is observed in images from the Nançay Radioheliograph (NRH; Kerdraon & Delouis 1997) at 150 and 173 MHz with a cadence of 0.25 s. Both split bands of the harmonic lane can be imaged at these two frequencies. To determine movement of the Type II sources, we extracted the centroids of the Type II emission by fitting an eliptical Gaussian to the radio sources and estimating the errors in centroid positions using the methods of Condon (1997); Morosan et al. (2019a). The elliptical Gaussian was fitted to radio contours with values over 107 K in brightness temperature which includes most of the extent of the radio sources observed.