Abstract
We performed the spectral analysis of Suzaku data on GT-Mus which was observed to emit 6.7 keV during its flaring period. GT-Mus was observed by the Suzaku team on December 12, 2007, with observation identity (402095010) for 96 kilo seconds. We downloaded GT-Mus data from the high energy astrophysics Suzaku archive. Our data reduction and analysis were done using XSELECT version 6.9 and XSPEC version 12.8. Errors reported in this work were done using the XPEC error command. We generated the spectrum and deduced a strong He-like (6.70 keV) emission from the source with Equivalent width of 282 ± 0.02 eV. This observed 6.7 keV emission line has an equivalent width which compares favorably with the equivalent width of 6.7 keV emission line from the galactic ridge (300-980 eV) depending on the Galactic position. From our analysis, we generated the light curve of the source which showed strong evidence of stellar flare. We therefore conclude that this observed stellar flare might be responsible for the observed 6.7 keV emission line. We however suggest that GT-Mus (HD101379) and other RS CVn stars that emit in 6.7 keV line could contribute to the 6.7 kev emission line from the galactic ridge during their flaring periods, since they exhibit the same level of chromospheric activities.
Highlights
Most red dwarf stars of late spectral type which increases in brightness within a few minutes are flares stars
Since GT-MUs (HD101379) is a member of RS CVn stars, we suggest that other RS CVn stars located at the galactic center which emit in 6.7 keV during their flaring periods could contribute to 6.7 Kev emissions from the galactic ridge due to their similar chromospheric activities
We carried out spectral analysis of GT-MUs (HD 101379), and resolved a strong 6.7 keV emission line, which was emitted as a result of flaring activities from the source
Summary
Most red dwarf stars of late spectral type which increases in brightness within a few minutes are flares stars. Chikwem Obinna Goodwill et al.: Contribution of GT-Mus to the 6.7 keV Emission Line from the Galactic Ridge observed [9,10,11,12,13].
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