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

Ogbodo O.O.V¹ , Chima A.I² , Onyia A.I³

Section:Research Paper, Product Type: Journal-Paper
Vol.7 , Issue.4 , pp.39-43, Aug-2019

CrossRef-DOI:   https://doi.org/10.26438/ijsrpas/v7i4.3943

Online published on Aug 31, 2019

Copyright © Ogbodo O.O.V, Chima A.I, Onyia A.I . This is an open access article distributed under the Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
 

View this paper at   Google Scholar | DPI Digital Library

XML View     PDF Download

How to Cite this Paper

420 Views    200 Downloads    98 Downloads

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.

Key-Words / Index Term :
Iron k-line, 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] Heintz, W. D. (1978). Double Stars. Dordrecht: D. Reidel Publishing Company. pp. 1–2.
[7] Jacobs, V. L., Decaux, V., & BeiersdorFer, P., (2004). X-ray Diagnostics of Astrophysical plasmas Cambridge, MA, United States.
[8] Kahn, S. M., Behar, E., Kinkhabwala, A., &Savin D. W., (2002). the Royal Society, 360, 1923.
[9] Boldt, E. (1987). Astronomy and astrophysics with the Advanced X-ray Astrophysics Facility. Physics Report 146:216.
[10] Eze, R. N. C, (2013). Fe K Alpha Line in Hard X- ray emitting symbiotic star Monthly Notices of the Royal Astronomical Society.
[11] Esaenwi, S., Eze, R.N.C., (2014). New Astronomy 2, Sol-gel synthesis, optical and structural characterization of ZrOS nanopowder.
[12]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.
[13] Piro, L., (1993). Iron K Line Diagnostics in Astrophysical Sources Press) adsabs Harvard edu 71993 yxrs. Oof. 4484.