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

Chikwem Obinna Goodwill; Esaenwi Sudum; Ambrose Chukwudi Eze

doi:doi:10.11648/j.ijhep.20190601.12

| Peer-Reviewed

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

Chikwem Obinna Goodwill, Esaenwi Sudum, Ambrose Chukwudi Eze

Published in International Journal of High Energy Physics (Volume 6, Issue 1)

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

Views: Downloads:

Download PDF

Share This Article

Twitter
Linked In
Facebook

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

[1]	Unsld, A 1957, IAU symposium Vol 4, 238-240.
[2]	Lovell, B; 1964 Observatory 84, 191.
[3]	Lovell, B; 1971 Quart. J. Roy Aston. Soc. 12, 98.
[4]	Gershberg, R.; 1970 in H. J. Habing (ed.) ‘interstellar gas dynamics’, IAU Symposium No.39, D. Reidel Publ. Co., Dordrecht, Holland, p. 305.
[5]	Tanaka Y 2002, A&A 382 1052.
[6]	Esaenwi, S., & Eze, R. N. C. (2015) On the origin of the Fe Kα Emission Line from Intermediate Polar EX Hyrae. New Astronomy, Volume 35, Pages 84-87.
[7]	Eze, A. C., Eze, R. N. C., & Esaenwi, S., (2017) On the contribution of the 6.7 keV line emission of the Algol binary system to the 6.7 keV from the galactic ridge. Turkish Journal of Physics, 41: 277-284. Doi: 10.3906/fiz-1703-1.
[8]	Hall D. S., 1976. IAU Coll.29, ed. W. S. Fitch. (Dordrecht: Reidel) p. 287.
[9]	Caillault, J. ApJ.1982, 87, 558.
[10]	Rengarajan, T. N., and Verma, R. P. Mon. Not. R. Astron. Soc 1983, 203, 1035.
[11]	Schrijver, C. J. Astron. Ap. 1983, 127, 289.
[12]	Schrijver, C. J., Mewe, R., and Walter, F. M. Astron. Ap. 1984, 138, 258.
[13]	Walter, F. M., Gibson, D. M., and Basri, G. S. Ap J. 1980, 267, 665.
[14]	Drake, S. A., Simon, T., and Linsky, J. L. A. J. 1986, 91, 1229.
[15]	Mitrou C. K., Mathioudakis M., Doyle J. G. and Antonopoulou E. Astran. Astrapbys. 1997,317,776.
[16]	Dempsey R. C., Linsky J. L., Fleming T. A. and Schmitt J. H'. M. M. ApJSS. 1993, 86, 599.
[17]	Gurzadyan G. A. and Cholakyan V. G. Ap&SS. 1995, 229, 185.
[18]	Murdoch K. A., Hearnshaw J. B., Kilmartin P. M., Gilmore A. C., 1995, Mon. NOT. R. Astron. Soc. 276,836.
[19]	McAlister, H., Hartkopf, W. I., & Franz, O. G. The Astron. J. 1990, 99, 978.
[20]	Koyama K, Makishima K, Tanaka, Y and Tsunemi H. PASJ. 1986, 38 121.
[21]	Koyama K, Maeda Y, Sonobe T, Takeshima T, Tanaka Y and Yamauchi S. PASJ.1996, 48 249.
[22]	Muno, M. P., Baganoff, F. K., Bautz, M. W., Brandt, W. N., Broos, P. S., Feigelson, E. D., & Townsley, L. K. The Astrophys. J. 2003, 589, 225.
[23]	Muno, M. P., Arabadjis, J. S., Baganoff, F. K., Bautz, M. W., Brandt, W. N., Broos, P. S.,& Ricker, G. R. The Astrophys. J. 2004 613, 11795.
[24]	Revnivtsev, M., Sazonov, S., Gilfanov, M., Churazov, E., & Sunyaev, R. A & A 2006, 452, 178.
[25]	K. Ebisawa., S. Yamauchi., Y. Tanaka., K. Koyama., Y. Ezoe., A. Bamba., M. Kokubun., Y. Hyodo., M. Tsuiimoto., H. Takahashi. Publ. Astrono. Soc. Japan.2008, S223.
[26]	T. Yuasa., K. Nakazawa., K. Makishima., K. Saitou., M. Ishida., k. Ebisawa., H. Mori and S. Yamada. A & A. 2010. A520, A25.
[27]	Yamauchi, S., Ebisawa, K., Tanaka, Y., Koyama, K., Matsumoto, H., Yamasaki, N. Y., & Yuichiro, E. Publ. Astrono. Soc. Japan. 2009, 61, S232.
[28]	Morihana K., Masahiro T., Tessei Y., and Ebisawa K. 2013, ApJ, 766, 14.

Cite This Article

Plain Text BibTeX RIS

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

Copy | Download

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

Copy | Download

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

Copy | Download

@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}
}

Copy | Download

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 -

Copy | Download

Author Information

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

Download PDF

Sections

Plain Text BibTeX RIS

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

Copy | Download

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

Copy | Download

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

Copy | Download

@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}
}

Copy | Download