| Name: Divya Paliwal |
| Affiliation: USO PRL Ahmedabad |
| Conference ID: ASI2026_850 |
| Title: A high-frequency type II radio burst associated with an X2.3 class flare |
| Abstract Type: Poster |
| Abstract Category: Sun, Solar System, Exoplanets, and Astrobiology |
| Author(s) and Co-Author(s) with Affiliation: Divya Paliwal(Udaipur Solar Observatory, Physical Research Laboratory, Udaipur, India), Vishwavijay Singh(Udaipur Solar Observatory, Physical Research Laboratory, Udaipur, India), Nadiya K(Mahatma Gandhi University, Kerala, Kottayam, India), Anshu Kumari(Udaipur Solar Observatory, Physical Research Laboratory, Udaipur, India) |
| Abstract: Radio observations provide access to the corona, heliosphere, and ionosphere, and are thought to be an excellent indicator of disturbances in the solar atmosphere. An immediate indicator of solar transients, such as solar flares and coronal mass ejections, is solar radio bursts, especially in the inner and middle corona. We studied a rare type II high-frequency (start frequency: ~750 MHz), fast-drifting (~0.5 MHz/s) type II radio burst on November 6, 2024. The active region source location for this burst was S08E14 (AR13883). There was an X2.3 class flare associated with this burst, which started at 13:24 UT, peaked at 13:40 UT, and ended at 13:46 UT. The duration of the X-ray flare was ~ 22 min. There was an EUV wave seen just after the flare at ~ 13:55 UT in the SDO-AIA field of view (fov). Several ground-based radio spectrographs had recorded this type II radio burst at 13:50 and 13:56 UT, spanning frequencies from ~ 750 MHz to 45 MHz. Radio imaging observations with the Nancay radio heliograph (NRH) in the frequency range of 444-150 MHz, corresponding to a height range of 1.01-1.29 R⊙, reveal that the radio sources were moving in the east direction. We used the High Energy L1 Orbiting X-Ray Spectrometer (HELIOS) on-board Aditya-L1 data for spectroscopy to find the cut-off energy range for non-thermal emission. We used the Spectrometer Telescope for Imaging X-rays (STIX) on board Solar Orbiter (SoLO) to locate the hard X-ray emission region at the eruption footpoints. Our preliminary analysis suggests that the type II bursts were not associated with any whitelight CME, as it was not sufficient to give rise to the shock in the inner corona. This Type II radio burst was associated with the flare blast wave generated due to the strong X2.3-class flare.
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