Contribution of GT-Mus to the 6.7 keV Emission Line from the Galactic Ridge
International Journal of High Energy Physics
Volume 6, Issue 1, June 2019, Pages: 13-16
Received: May 6, 2019; Accepted: Jun. 5, 2019; Published: Jun. 19, 2019
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Chikwem Obinna Goodwill, Department of Physics and Astronomy, University of Nigeria, Nsukka, Nigeria
Esaenwi Sudum, Department of Astronomy, NASRDA-Centre for Basic Space Science, Nsukka, Nigeria
Ambrose Chukwudi Eze, Department of Physics and Geosciences, Godfrey Okoye University, Enugu State, Nigeria
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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.
Flare Stars, RS CVn, Galactic Ridge X-ray Emission
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Chikwem Obinna Goodwill, Esaenwi Sudum, Ambrose Chukwudi Eze, Contribution of GT-Mus to the 6.7 keV Emission Line from the Galactic Ridge, International Journal of High Energy Physics. Vol. 6, No. 1, 2019, pp. 13-16. doi: 10.11648/j.ijhep.20190601.12
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