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Spectral and Timing Nature of the Symbiotic X-Ray Binary 4U 1954+319: The Slowest Rotating Neutron Star in AN X-Ray Binary System

Tamagawa, Toru ; Fuerst, Felix ; Marcu, Diana ; Wilms, Jorn ; Makishima, Kazuo ; Pottschmidt, Katja ; Yamada, Shin'Ya ; Corbet, Robin H. D. ; Enoto, Teruaki ; Sasano, Makoto; NASA Goddard Space Flight Center

The Astrophysical Journal; Volume 786; No. 2; 127 [Tạp chí có phản biện]

20150010753; GSFC-E-DAA-TN23866

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  • Nhan đề:
    Spectral and Timing Nature of the Symbiotic X-Ray Binary 4U 1954+319: The Slowest Rotating Neutron Star in AN X-Ray Binary System
  • Tác giả: Tamagawa, Toru ; Fuerst, Felix ; Marcu, Diana ; Wilms, Jorn ; Makishima, Kazuo ; Pottschmidt, Katja ; Yamada, Shin'Ya ; Corbet, Robin H. D. ; Enoto, Teruaki ; Sasano, Makoto
  • NASA Goddard Space Flight Center
  • Chủ đề: Astrophysics
  • Là 1 phần của: The Astrophysical Journal; Volume 786; No. 2; 127
  • Mô tả: The symbiotic X-ray binary (SyXB) 4U 1954+319 is a rare system hosting a peculiar neutron star (NS) and an M-type optical companion. Its approx. 5.4 hr NS spin period is the longest among all known accretion-powered pulsars and exhibited large (is approx. 7%) fluctuations over 8 yr. A spin trend transition was detected with Swift/BAT around an X-ray brightening in 2012. The source was in quiescent and bright states before and after this outburst based on 60 ks Suzaku observations in 2011 and 2012. The observed continuum is well described by a Comptonized model with the addition of a narrow 6.4 keV Fe-K alpha line during the outburst. Spectral similarities to slowly rotating pulsars in high-mass X-ray binaries, its high pulsed fraction (approx. 60%-80%), and the location in the Corbet diagram favor high B-field (approx. greater than 10(exp12) G) over a weak field as in low-mass X-ray binaries. The observed low X-ray luminosity (10(exp33)-10(exp35) erg s(exp1)), probable wide orbit, and a slow stellar wind of this SyXB make quasi-spherical accretion in the subsonic settling regime a plausible model. Assuming a approx. 10(exp13) G NS, this scheme can explain the approx. 5.4 hr equilibrium rotation without employing the magnetar-like field (approx. 10(exp16) G) required in the disk accretion case. The timescales of multiple irregular flares (approx. 50 s) can also be attributed to the free-fall time from the Alfven shell for a approx. 10(exp13) G field. A physical interpretation of SyXBs beyond the canonical binary classifications is discussed.
  • Năm xuất bản: 2014
  • Ngôn ngữ: English
  • Số nhận dạng: 20150010753; GSFC-E-DAA-TN23866

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