Abstract Details
| Name: Pramod Kumar Affiliation: Jagan Nath University, Jaipur Conference ID: ASI2015_387 Title : X-ray emission characteristics of a solar flare observed on 05 April 2004 Authors and Co-Authors : Rajmal Jain1, Pramod Kumar2, Arun K. Awasthi3, Nipa J. Bhatt4 and Yogesh C. Bhatt2 1Kadi Sarwa Viswavidhalaya, Gandhinagar 392012, India 2Jagan Nath University, Jaipur 303901, India 3Institute of Astronomy, University of Wroclaw, Wroclaw, Poland 4C. U. Shah Science College, Ahmadabad 380014, India Abstract Type : Poster Abstract Category : Sun and the Solar System Abstract : We present temporal and spectral characteristics of X-ray emission from a solar flare observed on 05 April 2004 by the Si detector onboard the Solar X-ray Spectrometer (SOXS) mission. SOXS was flown onboard GSAT-2 Indian spacecraft on 08 May 2003. The flare began at 05:35:30 UT and decayed after 06:30 UT in 4-5 keV energy band. The flare has been observed in 4-20 keV energy range. Temporal characteristics of flare evolution as a function of energy band have been studied in 4-20 keV with the step of 1 keV energy interval. Considering 5 rise relative to background we find the flare begins first in 4-5 keV but lasts for the longest period than any higher energy band under study. Temporal characteristics suggest that the flare duration in 4-5 keV is longest and keeps on reducing in next higher and higher energy bands. We study in detail the peak time delay as a function of energy interval of 1 keV to investigate the conductive and radiative cooling time scales during the flare. The spectral characteristics are presented of the flare emission in the 4-20 keV energy range. The spectral fits allow us to measure the peak flare temperature, differential emission measure (DEM) and the thermal power-law index employing least-χ2 fitting. We carried out forward fit of the count spectra opting CHIANTI code inside the OSPEX and de-convolving over the response matrix. We obtained differential emission measure (DEM) in the range 0.008-0.09 X 1049/cm3 keV; peak flare plasma temperature between 10-20MK and multi-thermal power-law spectral index varying 4.50-7.20. The negative power law spectral index varies between 2.3 and 6.5. The RHESSI mission provides imaging of the flare soft and hard X-ray components and enables us to measure the location and the size of the loops. The half loop length has been estimated to be 30000 km. Key worlds: Solar Flare, X ray emissions, SOXS, Spectral analysis, Spectral parameters |