2011/09/05 by K. L. Li, Li, K. L., Chun. S. J. Pun +1
Physics and Astronomy · #FOS: Physical sciences #High Energy Astrophysical Phenomena (astro-ph.HE) #astro-ph.HE
paper · pdf · doi:10.48550/arxiv.1109.0982
arxiv created 2011/09/05 · arxiv updated 2011/09/06
We present a study of a young (few years old) supernova remnant 2003lx which was first discovered in X-ray through two serendipitous Swift observations in 2008 January and the corresponding merged image revealed a 7σsource detection at 2.1±1.2 arcsec (0.9 +/- 0.5 Swift pixels) from the optical position of the supernova. The X-ray luminosity Lx = 4.8-1.7+1.8 × 1041 erg/s of band 0.3 - 2.0 keV is estimated by a redshift z = 0.0377 power law which can infer a companion star with a mass-loss rate of M ~ 10-4 M_\sun per year (with assumption of wind velocity vw = 10 km/s) in the white dwarf binary system. Thermal Model fitting suggests the temperature of the shock wave front is kT ~ 0.4 keV which is consistent with the typical reverse shock temperate. The X-ray emission allows us to probe the interaction between the fast moving debris of the exploded star and the circumstellar medium (CSM). This in turns provides footprints of the mass-loss history of the exploded system, and may allow us to learn about the nature of the progenitor and its companion.