Variable absorption line in XTE J1810-197 |
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| Affiliation: | 1. Department of Astronomy and Space Sciences, Graduate School of Science and Engineering, İstanbul University, Beyazıt, İstanbul 34116, Turkey;2. Faculty of Engineering and Natural Sciences, Sabancı University, Tuzla, İstanbul 34956, Turkey;3. Center of Astronomy, Indian Institute of Technology Indore, Khandwa Road, Simrol, Indore 453552, India;4. Department of Astronomy and Space Sciences, Science Faculty, İstanbul University, Beyazıt, İstanbul 34119, Turkey;5. İstanbul University Observatory Research and Application Center, Istanbul University, İstanbul 34119, Turkey;1. Astrophysical Sciences Division, Bhabha Atomic Research Centre, Mumbai 400 085, India;2. Homi Bhabha National Institute, Anushaktinagar, Mumbai 400 094, India;1. Laboratório Nacional de Astrofísica, Rua Estados Unidos, 154, CEP, Itajubá, MG 37504-364 Brazil;2. CBA Wisconsin, Luckydog Observatory, 65027 Howath Road, de Soto, WI 54624, USA;3. CBA Concord, 1730 Helix Ct., Concord, CA 94518, USA;4. CBA Ontario, Newcastle Observatory, 9 Laking Drive, Newcastle, ON L1B 1M5, Canada;5. AAVSO, Rolling Hills Observatory, 1643 Nightfall Drive, Clermont, FL 34711, USA;6. CBA Oregon, Jack Jones Observatory, 22665 Bents Road NE, Aurora, OR 97002, USA;7. CBA Wilts, 2 Spa Close, Highworth, Swingdon SN6 7PJ, UK;8. CBA Sierras, Sierra Remote Observatories, 44325 Alder Heights Road, Auberry, CA 93602, USA;9. CBA Illinois, Northbrook Meadow Observatory, 855 Fair Lane, Northbrook, IL 60062, USA |
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| Abstract: | We report the results of a long-term spectral and timing study of the first transient magnetar, XTE J1810-197 which was discovered in 2003, when its X-ray luminosity increased ≈ 100 fold. We fit X-ray spectra of all archival X-ray observations using a two-component blackbody model, where the cool component is most likely originating from the whole surface of the neutron star and the hot component is from a much smaller hot spot. We investigate the long-term evolution of the surface emission characteristics via tracing its surface temperature, apparent emitting area and pulsed fraction. We evaluate the pulsed fraction in two energy intervals ( < 1.5 keV and > 1.5 keV) and show that the XTE J1810-197 exhibits slightly higher pulsed emission at energies above 1.5 keV. We explore the characteristics of an absorption line detected around 1.1 keV. We find that the absorption feature is highly variable and its profile is asymmetric. To accurately represent this feature, we introduced an asymmetric Gaussian profile, and quantified the level of asymmetry of the absorption feature. |
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