Interpretation of Quiescent Behavior of Iron K-alpha (Fe Kα) Emission Line from Sigma Gem

Ogbodo Osondu Vivian; Chima Abraham Iheanyichukwu; Onyia Augustine Ike

doi:doi:10.11648/j.ijhep.20200701.13

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Interpretation of Quiescent Behavior of Iron K-alpha (Fe Kα) Emission Line from Sigma Gem

Ogbodo Osondu Vivian, Chima Abraham Iheanyichukwu, Onyia Augustine Ike

Published in International Journal of High Energy Physics (Volume 7, Issue 1)

Received: 10 May 2019 Accepted: 10 June 2019 Published: 6 July 2020

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Abstract

In this research the interpretation of Suzaku spectral observation of Fe kα emission line from Sigma Gem system was carried out. Sigma Gem was observed using Suzaku satellite with observation ID 402033010 at an exposure time of 142. 82 ks. Spectral analysis of all observations was performed using XSPEC version 12.8. We used version 2.00 of the standard Suzaku pipeline products and the HEA Soft version 6.16 for our analysis of data. We adopted a 250′′ radius to extract all events for the XIS detector to produce the source spectra, but we adjusted the 250′′ radius slightly where it overlaps with the calibration sources at the corners, to avoid capturing source background light. Modeling the spectrum using either power law or bremsstrahlung model with three Gaussian line for the 6.4 keV, He–like 6.7 keV, H–like 7.0 keV, Fe Kα emission lines shows that the 6.4 keV, 7.0 keV lines and absorption in both full and partial covering matter could not be measured in all the sources. We were able to resolve the three-narrow iron kα emission lines with different ionization states, which constraints the Sigma Gem emission models. The iron K- line complex was clearly resolved into three individual peaks at 6.41 keV, 6.7 keV and 7.0 keV. The light curve shows that the Sigma Gem was at a quiescent state at the point of observation and The light curve shows a considerable quiescent behavior of the source of the point of observation showing the source is not flaring.

Published in	International Journal of High Energy Physics (Volume 7, Issue 1)
DOI	10.11648/j.ijhep.20200701.13
Page(s)	15-18
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), 2024. Published by Science Publishing Group

Keywords

Iron, X-ray, Sigma Gen

References

[1]	Aizu, K. (1973). X-Ray Emission Region of a White Dwarf with Accretion Theoretical physics, journal letter vol. 49, no. 1184.
[2]	Mitchell, R. J, Culhane, J. L Davison, P. J., & Ivesm J. C., (1976). Monthly Notices of the Radio Astronomy Society, 176, 29.
[3]	Makishimak, (1986). in Mason K. O., Watson M. G., White N. E. eds the physics of accretion onto compact objects. Springer-Verlag, Berlin, p. 249.
[4]	Hellier, C., Mason, K. O., Rosen, S. R., & Cordova, F. A. (1989). Accretion-powered Compact BinariesMonthly Notices of the Radio Astronomy Society, 228, 463.
[5]	Helliler, C., (2001). Cataclysmic variable stars-how and why they vary, Springer Science and Business media, New York.
[6]	Heller, C., (1997). Monthly Notices of the Royal Astronomical Society, 291, 71.
[7]	Heintz, W. D. (1978). Double Stars. Dordrecht: D. Reidel Publishing Company. pp. 1–2.
[8]	Hubber, D. A. A. P. Whitworth (2005). "Binary Star Formation from Ring Fragmentation". Astronomy & Astrophysics. 437: 113–125
[9]	Jacobs, V. L., Decaux, V., & BeiersdorFer, P., (2004). X-ray Diagnostics of Astrophysical plasmas Cambridge, MA, United States.
[10]	Kahn, S. M., Behar, E., Kinkhabwala, A., &Savin D. W., (2002). the Royal Society, 360, 1923.
[11]	Boldt, E. (1987). Astronomy and astrophysics with the Advanced X-ray Astrophysics Facility. Physics Report 146: 216.
[12]	Eze, R. N. C, (2013). Fe K Alpha Line in Hard X- ray emitting symbiotic star Monthly Notices of the Royal Astronomical Society.
[13]	Esaenwi, S., Eze, R. N. C., (2014). New Astronomy 2, Sol-gel synthesis, optical and structural characterization of ZrOS nanopowder.
[14]	Massarotti, Alessandra Latham, David W. Stefamik, Robert P. Fogel, Jeffery. (2008). Rotational and Radial velocities for a sample of 761 HIPPARCOS Giants and the Role of Binarity.
[15]	Matranga, M.; Drake, J. J.; Kashyap, V. L.; Marengo, M. Kuchner, M. J. (2010). Close Binaries with Infrared Excess: Destroyers of Worlds, The Astrophysical Journal Letters, Volume 720, Issue 2, L164-L168.
[16]	Piro, L., (1993). Iron K Line Diagnostics in Astrophysical Sources Press) adsabs Harvard edu 71993 yxrs. Oof. 4484.

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Ogbodo Osondu Vivian, Chima Abraham Iheanyichukwu, Onyia Augustine Ike. (2020). Interpretation of Quiescent Behavior of Iron K-alpha (Fe Kα) Emission Line from Sigma Gem. International Journal of High Energy Physics, 7(1), 15-18. https://doi.org/10.11648/j.ijhep.20200701.13

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ACS Style

Ogbodo Osondu Vivian; Chima Abraham Iheanyichukwu; Onyia Augustine Ike. Interpretation of Quiescent Behavior of Iron K-alpha (Fe Kα) Emission Line from Sigma Gem. Int. J. High Energy Phys. 2020, 7(1), 15-18. doi: 10.11648/j.ijhep.20200701.13

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Ogbodo Osondu Vivian, Chima Abraham Iheanyichukwu, Onyia Augustine Ike. Interpretation of Quiescent Behavior of Iron K-alpha (Fe Kα) Emission Line from Sigma Gem. Int J High Energy Phys. 2020;7(1):15-18. doi: 10.11648/j.ijhep.20200701.13

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@article{10.11648/j.ijhep.20200701.13,
  author = {Ogbodo Osondu Vivian and Chima Abraham Iheanyichukwu and Onyia Augustine Ike},
  title = {Interpretation of Quiescent Behavior of Iron K-alpha (Fe Kα) Emission Line from Sigma Gem},
  journal = {International Journal of High Energy Physics},
  volume = {7},
  number = {1},
  pages = {15-18},
  doi = {10.11648/j.ijhep.20200701.13},
  url = {https://doi.org/10.11648/j.ijhep.20200701.13},
  eprint = {https://article.sciencepublishinggroup.com/pdf/10.11648.j.ijhep.20200701.13},
  abstract = {In this research the interpretation of Suzaku spectral observation of Fe kα emission line from Sigma Gem system was carried out. Sigma Gem was observed using Suzaku satellite with observation ID 402033010 at an exposure time of 142. 82 ks. Spectral analysis of all observations was performed using XSPEC version 12.8. We used version 2.00 of the standard Suzaku pipeline products and the HEA Soft version 6.16 for our analysis of data. We adopted a 250′′ radius to extract all events for the XIS detector to produce the source spectra, but we adjusted the 250′′ radius slightly where it overlaps with the calibration sources at the corners, to avoid capturing source background light. Modeling the spectrum using either power law or bremsstrahlung model with three Gaussian line for the 6.4 keV, He–like 6.7 keV, H–like 7.0 keV, Fe Kα emission lines shows that the 6.4 keV, 7.0 keV lines and absorption in both full and partial covering matter could not be measured in all the sources. We were able to resolve the three-narrow iron kα emission lines with different ionization states, which constraints the Sigma Gem emission models. The iron K- line complex was clearly resolved into three individual peaks at 6.41 keV, 6.7 keV and 7.0 keV. The light curve shows that the Sigma Gem was at a quiescent state at the point of observation and The light curve shows a considerable quiescent behavior of the source of the point of observation showing the source is not flaring.},
 year = {2020}
}

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TY  - JOUR
T1  - Interpretation of Quiescent Behavior of Iron K-alpha (Fe Kα) Emission Line from Sigma Gem
AU  - Ogbodo Osondu Vivian
AU  - Chima Abraham Iheanyichukwu
AU  - Onyia Augustine Ike
Y1  - 2020/07/06
PY  - 2020
N1  - https://doi.org/10.11648/j.ijhep.20200701.13
DO  - 10.11648/j.ijhep.20200701.13
T2  - International Journal of High Energy Physics
JF  - International Journal of High Energy Physics
JO  - International Journal of High Energy Physics
SP  - 15
EP  - 18
PB  - Science Publishing Group
SN  - 2376-7448
UR  - https://doi.org/10.11648/j.ijhep.20200701.13
AB  - In this research the interpretation of Suzaku spectral observation of Fe kα emission line from Sigma Gem system was carried out. Sigma Gem was observed using Suzaku satellite with observation ID 402033010 at an exposure time of 142. 82 ks. Spectral analysis of all observations was performed using XSPEC version 12.8. We used version 2.00 of the standard Suzaku pipeline products and the HEA Soft version 6.16 for our analysis of data. We adopted a 250′′ radius to extract all events for the XIS detector to produce the source spectra, but we adjusted the 250′′ radius slightly where it overlaps with the calibration sources at the corners, to avoid capturing source background light. Modeling the spectrum using either power law or bremsstrahlung model with three Gaussian line for the 6.4 keV, He–like 6.7 keV, H–like 7.0 keV, Fe Kα emission lines shows that the 6.4 keV, 7.0 keV lines and absorption in both full and partial covering matter could not be measured in all the sources. We were able to resolve the three-narrow iron kα emission lines with different ionization states, which constraints the Sigma Gem emission models. The iron K- line complex was clearly resolved into three individual peaks at 6.41 keV, 6.7 keV and 7.0 keV. The light curve shows that the Sigma Gem was at a quiescent state at the point of observation and The light curve shows a considerable quiescent behavior of the source of the point of observation showing the source is not flaring.
VL  - 7
IS  - 1
ER  -

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Author Information

Ogbodo Osondu Vivian

Department of Industrial Physics, Enugu State University of Science and Technology, Enugu, Nigeria
Chima Abraham Iheanyichukwu

Department of Industrial Physics, Enugu State University of Science and Technology, Enugu, Nigeria
Onyia Augustine Ike

Department of Industrial Physics, Enugu State University of Science and Technology, Enugu, Nigeria

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Ogbodo Osondu Vivian, Chima Abraham Iheanyichukwu, Onyia Augustine Ike. (2020). Interpretation of Quiescent Behavior of Iron K-alpha (Fe Kα) Emission Line from Sigma Gem. International Journal of High Energy Physics, 7(1), 15-18. https://doi.org/10.11648/j.ijhep.20200701.13

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ACS Style

Ogbodo Osondu Vivian; Chima Abraham Iheanyichukwu; Onyia Augustine Ike. Interpretation of Quiescent Behavior of Iron K-alpha (Fe Kα) Emission Line from Sigma Gem. Int. J. High Energy Phys. 2020, 7(1), 15-18. doi: 10.11648/j.ijhep.20200701.13

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AMA Style

Ogbodo Osondu Vivian, Chima Abraham Iheanyichukwu, Onyia Augustine Ike. Interpretation of Quiescent Behavior of Iron K-alpha (Fe Kα) Emission Line from Sigma Gem. Int J High Energy Phys. 2020;7(1):15-18. doi: 10.11648/j.ijhep.20200701.13

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@article{10.11648/j.ijhep.20200701.13,
  author = {Ogbodo Osondu Vivian and Chima Abraham Iheanyichukwu and Onyia Augustine Ike},
  title = {Interpretation of Quiescent Behavior of Iron K-alpha (Fe Kα) Emission Line from Sigma Gem},
  journal = {International Journal of High Energy Physics},
  volume = {7},
  number = {1},
  pages = {15-18},
  doi = {10.11648/j.ijhep.20200701.13},
  url = {https://doi.org/10.11648/j.ijhep.20200701.13},
  eprint = {https://article.sciencepublishinggroup.com/pdf/10.11648.j.ijhep.20200701.13},
  abstract = {In this research the interpretation of Suzaku spectral observation of Fe kα emission line from Sigma Gem system was carried out. Sigma Gem was observed using Suzaku satellite with observation ID 402033010 at an exposure time of 142. 82 ks. Spectral analysis of all observations was performed using XSPEC version 12.8. We used version 2.00 of the standard Suzaku pipeline products and the HEA Soft version 6.16 for our analysis of data. We adopted a 250′′ radius to extract all events for the XIS detector to produce the source spectra, but we adjusted the 250′′ radius slightly where it overlaps with the calibration sources at the corners, to avoid capturing source background light. Modeling the spectrum using either power law or bremsstrahlung model with three Gaussian line for the 6.4 keV, He–like 6.7 keV, H–like 7.0 keV, Fe Kα emission lines shows that the 6.4 keV, 7.0 keV lines and absorption in both full and partial covering matter could not be measured in all the sources. We were able to resolve the three-narrow iron kα emission lines with different ionization states, which constraints the Sigma Gem emission models. The iron K- line complex was clearly resolved into three individual peaks at 6.41 keV, 6.7 keV and 7.0 keV. The light curve shows that the Sigma Gem was at a quiescent state at the point of observation and The light curve shows a considerable quiescent behavior of the source of the point of observation showing the source is not flaring.},
 year = {2020}
}

Copy | Download

TY  - JOUR
T1  - Interpretation of Quiescent Behavior of Iron K-alpha (Fe Kα) Emission Line from Sigma Gem
AU  - Ogbodo Osondu Vivian
AU  - Chima Abraham Iheanyichukwu
AU  - Onyia Augustine Ike
Y1  - 2020/07/06
PY  - 2020
N1  - https://doi.org/10.11648/j.ijhep.20200701.13
DO  - 10.11648/j.ijhep.20200701.13
T2  - International Journal of High Energy Physics
JF  - International Journal of High Energy Physics
JO  - International Journal of High Energy Physics
SP  - 15
EP  - 18
PB  - Science Publishing Group
SN  - 2376-7448
UR  - https://doi.org/10.11648/j.ijhep.20200701.13
AB  - In this research the interpretation of Suzaku spectral observation of Fe kα emission line from Sigma Gem system was carried out. Sigma Gem was observed using Suzaku satellite with observation ID 402033010 at an exposure time of 142. 82 ks. Spectral analysis of all observations was performed using XSPEC version 12.8. We used version 2.00 of the standard Suzaku pipeline products and the HEA Soft version 6.16 for our analysis of data. We adopted a 250′′ radius to extract all events for the XIS detector to produce the source spectra, but we adjusted the 250′′ radius slightly where it overlaps with the calibration sources at the corners, to avoid capturing source background light. Modeling the spectrum using either power law or bremsstrahlung model with three Gaussian line for the 6.4 keV, He–like 6.7 keV, H–like 7.0 keV, Fe Kα emission lines shows that the 6.4 keV, 7.0 keV lines and absorption in both full and partial covering matter could not be measured in all the sources. We were able to resolve the three-narrow iron kα emission lines with different ionization states, which constraints the Sigma Gem emission models. The iron K- line complex was clearly resolved into three individual peaks at 6.41 keV, 6.7 keV and 7.0 keV. The light curve shows that the Sigma Gem was at a quiescent state at the point of observation and The light curve shows a considerable quiescent behavior of the source of the point of observation showing the source is not flaring.
VL  - 7
IS  - 1
ER  -

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