| 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: | Asif M. Mandayapuram 1 , Mehul R. Pandya 1 , Mithun N.P.S 2 , Santosh V. Vadawale 2 ,Thomas N. Woods 3 |
| Authors Affiliation: | 1. Space Sciences Division, Space Applications Centre, Indian Space Research Organisation,
Ahmedabad, 380015, India
2. Physical Research Laboratory, Navrangpura, Ahmedabad, Gujarat-380009, India
3. Laboratory for Atmospheric and Space Physics, University of Colorado at Boulder, 3665 Discovery
Dr., Boulder, CO 80303 |
| Mode of Presentation: | 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. |
