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SyXB형 4U 1954+319의 스펙트럼 및 시간적 특성 : X선 쌍성계에 속한 천천히 회전하는 중성자별

SPECTRAL AND TIMING NATURE OF THE SYMBIOTIC X-RAY BINARY 4U 1954+319: THE SLOWEST ROTATING NEUTRON STAR IN AN X-RAY BINARY SYSTEM
  • 작성자 : KASI
  • 작성일 : 2014-06-25
  • 조회수 : 3802
  • 저자Teruaki Enoto, Makoto Sasano, Shin'ya Yamada, Toru Tamagawa, Kazuo Makishima, Katja Pottschmidt, Diana Marcu, Robin H. D. Corbet, Felix Fuerst, and Jorn Wilms
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    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 ~5.4 hr NS spin period is the longest among all known accretion-powered pulsars and exhibited large (~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-Kα line during the outburst. Spectral similarities to slowly rotating pulsars in high-mass X-ray binaries, its high pulsed fraction (~60%-80%), and the location in the Corbet diagram favor high B-field ( 1012 G) over a weak field as in low-mass X-ray binaries. The observed low X-ray luminosity (1033-1035 erg s?1), 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 ~1013 G NS, this scheme can explain the ~5.4 hr equilibrium rotation without employing the magnetar-like field (~1016 G) required in the disk accretion case. The timescales of multiple irregular flares (~50 s) can also be attributed to the free-fall time from the Alfven shell for a ~1013 G field. A physical interpretation of SyXBs beyond the canonical binary classifications is discussed. 


  • 게재정보THE ASTROPHYSICAL JOURNAL(2014.05.10)에 실린 연구논문을 게시함
  • 첨부파일
  • 원 문http://iopscience.iop.org/0004-637X/786/2/127/
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