State transitions of GRS 1739−278 in the 2014 outburst

Sili Wang, Nobuyuki Kawai, Megumi Shidatsu, Yutaro Tachibana, Taketoshi Yoshii, Masayuki Sudo, Aya Kubota

研究成果: Article

1 引用 (Scopus)

抄録

We report on the X-ray spectral analysis and time evolution of GRS 1739−278 during its 2014 outburst, based on MAXI/GSC and Swift/XRT observations. Over the course of the outburst, a transition from the low/hard state to the high/soft state and then back to the low/hard state was seen. During the high/soft state, the innermost disk temperature mildly decreased, while the innermost radius estimated with the multi-color disk model remained constant at ∼18 (D/8.5 kpc)(cos i/cos 30◦)−1/2 km, where D is the source distance and i is the inclination of observation. This small innermost radius of the accretion disk suggests that the central object is more likely to be a Kerr black hole rather than a Schwardzschild black hole. Applying a relativistic disk emission model to the high/soft state spectra, a mass upper limit of 18.3 M was obtained based on the inclination limit i < 60◦ for an assumed distance of 8.5 kpc. Using the empirical relation of the transition luminosity to the Eddington limit, the mass is constrained to 4.0–18.3 M for the same distance. The mass can be further constrained to be no larger than 9.5 M by adopting the constraints based on the fits to the NuSTAR spectra with relativistically blurred disk reflection models (Miller et al. 2015, ApJ, 799, L6).

元の言語English
記事番号psy058
ジャーナルPublications of the Astronomical Society of Japan
巻70
発行部数4
DOI
出版物ステータスPublished - 2018 8 1
外部発表Yes

Fingerprint

outburst
inclination
spectral analysis
radii
accretion
accretion disks
spectrum analysis
luminosity
color
temperature
x rays

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

これを引用

State transitions of GRS 1739−278 in the 2014 outburst. / Wang, Sili; Kawai, Nobuyuki; Shidatsu, Megumi; Tachibana, Yutaro; Yoshii, Taketoshi; Sudo, Masayuki; Kubota, Aya.

：: Publications of the Astronomical Society of Japan, 巻 70, 番号 4, psy058, 01.08.2018.

研究成果: Article

Wang, S, Kawai, N, Shidatsu, M, Tachibana, Y, Yoshii, T, Sudo, M & Kubota, A 2018, 'State transitions of GRS 1739−278 in the 2014 outburst', Publications of the Astronomical Society of Japan, 巻. 70, 番号 4, psy058. https://doi.org/10.1093/pasj/psy058
Wang S, Kawai N, Shidatsu M, Tachibana Y, Yoshii T, Sudo M その他. State transitions of GRS 1739−278 in the 2014 outburst. Publications of the Astronomical Society of Japan. 2018 8 1;70(4). psy058. https://doi.org/10.1093/pasj/psy058
Wang, Sili ; Kawai, Nobuyuki ; Shidatsu, Megumi ; Tachibana, Yutaro ; Yoshii, Taketoshi ; Sudo, Masayuki ; Kubota, Aya. / State transitions of GRS 1739−278 in the 2014 outburst. ：: Publications of the Astronomical Society of Japan. 2018 ; 巻 70, 番号 4.
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AU - Kubota, Aya

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AB - We report on the X-ray spectral analysis and time evolution of GRS 1739−278 during its 2014 outburst, based on MAXI/GSC and Swift/XRT observations. Over the course of the outburst, a transition from the low/hard state to the high/soft state and then back to the low/hard state was seen. During the high/soft state, the innermost disk temperature mildly decreased, while the innermost radius estimated with the multi-color disk model remained constant at ∼18 (D/8.5 kpc)(cos i/cos 30◦)−1/2 km, where D is the source distance and i is the inclination of observation. This small innermost radius of the accretion disk suggests that the central object is more likely to be a Kerr black hole rather than a Schwardzschild black hole. Applying a relativistic disk emission model to the high/soft state spectra, a mass upper limit of 18.3 M was obtained based on the inclination limit i < 60◦ for an assumed distance of 8.5 kpc. Using the empirical relation of the transition luminosity to the Eddington limit, the mass is constrained to 4.0–18.3 M for the same distance. The mass can be further constrained to be no larger than 9.5 M by adopting the constraints based on the fits to the NuSTAR spectra with relativistically blurred disk reflection models (Miller et al. 2015, ApJ, 799, L6).

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