Abstract Details

Name: Asif Mohamed Mandayapuram
Affiliation: Space Applications Centre (ISRO)
Conference ID: ASI2025_361
Title : Simultaneous observations of elemental abundance evolution during solar flares using InspireSat-1 DAXSS and Chandrayaan-2 XSM
Authors and Co-Authors : Asif M. Mandayapuram 1 , Mehul R. Pandya 1 , Mithun N.P.S 2 , Santosh V. Vadawale 2 ,Thomas N. Woods 3
Abstract Type : Poster
Abstract Category : Sun, Solar System, Exoplanets, and Astrobiology
Abstract : Solar Flares are powerful bursts of radiation from the solar atmosphere caused by the sudden reorganization of magnetic topology. Soft X-ray (0.1-10 nm) spectroscopic observation is an excellent probe for the elemental composition of 5-30 MK plasma formed during solar flares. The time cadence and sensitivity of soft X-ray spectroscopic instruments such as InspireSat-1 Dual Aperture X-ray Solar Spectrometer (DAXSS) and Chandrayaan-2 Solar X-ray Monitor (XSM) make it possible to investigate the evolution of plasma during various phases of the flare, in particular how the abundances of low First Ionisation Potential (FIP) elements vary during solar flare. Here, we investigate how various flare parameters, namely flare temperature, emission measure, and elemental abundances, vary during the flare for a sample of 15 flares ( C to M class) that have simultaneous X-ray spectroscopic observations from DAXSS and XSM. X-ray spectra during flares are modeled as the sum of emissions from two isothermal temperature components with common elemental composition to obtain estimates of abundances of Mg, Si, S, Ar, Ca, and Fe along with the temperature and emission measure of individual components. We find that the temperature, emission measure, and variation in elemental abundances, as estimated from DAXSS and XSM, agree quite well for most of the studied flares. Our results show that the elemental abundances show a decrease from coronal values and towards photospheric values for low-FIP elements at the peak of the flare and start to recover during the decay phase of the flare, similar to recent previous reports for smaller events. We discuss the analysis results and their implications for understanding processes such as chromospheric evaporation during solar flares.