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Contribution of GT-Mus to the 6.7 keV Emission Line from the Galactic Ridge

Received: 6 May 2019     Accepted: 5 June 2019     Published: 19 June 2019
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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.

Published in International Journal of High Energy Physics (Volume 6, Issue 1)
DOI 10.11648/j.ijhep.20190601.12
Page(s) 13-16
Creative Commons

This is an Open Access article, distributed under the terms of the Creative Commons Attribution 4.0 International License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted use, distribution and reproduction in any medium or format, provided the original work is properly cited.

Copyright

Copyright © The Author(s), 2019. Published by Science Publishing Group

Keywords

Flare Stars, RS CVn, Galactic Ridge X-ray Emission

References
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  • APA Style

    Chikwem Obinna Goodwill, Esaenwi Sudum, Ambrose Chukwudi Eze. (2019). Contribution of GT-Mus to the 6.7 keV Emission Line from the Galactic Ridge. International Journal of High Energy Physics, 6(1), 13-16. https://doi.org/10.11648/j.ijhep.20190601.12

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    ACS Style

    Chikwem Obinna Goodwill; Esaenwi Sudum; Ambrose Chukwudi Eze. Contribution of GT-Mus to the 6.7 keV Emission Line from the Galactic Ridge. Int. J. High Energy Phys. 2019, 6(1), 13-16. doi: 10.11648/j.ijhep.20190601.12

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    AMA Style

    Chikwem Obinna Goodwill, Esaenwi Sudum, Ambrose Chukwudi Eze. Contribution of GT-Mus to the 6.7 keV Emission Line from the Galactic Ridge. Int J High Energy Phys. 2019;6(1):13-16. doi: 10.11648/j.ijhep.20190601.12

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  • @article{10.11648/j.ijhep.20190601.12,
      author = {Chikwem Obinna Goodwill and Esaenwi Sudum and Ambrose Chukwudi Eze},
      title = {Contribution of GT-Mus to the 6.7 keV Emission Line from the Galactic Ridge},
      journal = {International Journal of High Energy Physics},
      volume = {6},
      number = {1},
      pages = {13-16},
      doi = {10.11648/j.ijhep.20190601.12},
      url = {https://doi.org/10.11648/j.ijhep.20190601.12},
      eprint = {https://article.sciencepublishinggroup.com/pdf/10.11648.j.ijhep.20190601.12},
      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.},
     year = {2019}
    }
    

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  • TY  - JOUR
    T1  - Contribution of GT-Mus to the 6.7 keV Emission Line from the Galactic Ridge
    AU  - Chikwem Obinna Goodwill
    AU  - Esaenwi Sudum
    AU  - Ambrose Chukwudi Eze
    Y1  - 2019/06/19
    PY  - 2019
    N1  - https://doi.org/10.11648/j.ijhep.20190601.12
    DO  - 10.11648/j.ijhep.20190601.12
    T2  - International Journal of High Energy Physics
    JF  - International Journal of High Energy Physics
    JO  - International Journal of High Energy Physics
    SP  - 13
    EP  - 16
    PB  - Science Publishing Group
    SN  - 2376-7448
    UR  - https://doi.org/10.11648/j.ijhep.20190601.12
    AB  - 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.
    VL  - 6
    IS  - 1
    ER  - 

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Author Information
  • Department of Physics and Astronomy, University of Nigeria, Nsukka, Nigeria

  • Department of Astronomy, NASRDA-Centre for Basic Space Science, Nsukka, Nigeria

  • Department of Physics and Geosciences, Godfrey Okoye University, Enugu State, Nigeria

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