Hard-tail emission in the soft state of low-mass X-ray binaries and their relation to the neutron star magnetic field

DOI PDF 参考文献43件

書誌事項

公開日
2016-05-31
資源種別
journal article
DOI
  • 10.1093/pasj/psw048
公開者
Oxford University Press (OUP)

この論文をさがす

説明

<jats:title>Abstract</jats:title> <jats:p>Average hard-tail X-ray emission in the soft state of nine bright Atoll low-mass X-ray binaries containing a neutron star (NS-LMXBs) are investigated by using the light curves of MAXI/GSC (Gas Slit Camera) and Swift/BAT (Burst Alert Telescope). Two sources (4U 1820−30 and 4U 1735−44) exhibit a large hardness ratio (15–50 keV/2–10 keV: HR &gt;0.1), while the other sources distribute at HR ≲ 0.1. In either case, HR does not depend on the 2–10 keV luminosity. Therefore the difference of HR is due to the 15–50 keV luminosity, which is Comptonized emission. The Compton cloud is assumed to be around the neutron star. The size of the Compton cloud would affect the value of HR. Although the magnetic field of an NS-LMXB is weak, we could expect a larger Alfvén radius than the innermost stable circular orbit or the neutron star radius in some sources. In such cases, the accretion inflow is stopped at the Alfvén radius and would create a relatively large Compton cloud. This would result in the observed larger Comptonized emission. By attributing the difference of the size of Compton cloud to the Alfvén radius, we can estimate the magnetic fields of neutron stars. The obtained lower/upper limits are consistent with the previous results.</jats:p>

収録刊行物

参考文献 (43)*注記

もっと見る

関連プロジェクト

もっと見る

詳細情報 詳細情報について

問題の指摘

ページトップへ