具有最短轨道周期的超巨星快速X射线瞬变：朱雀观测到IGRJ16479-4514中的一个轨道
The Supergiant Fast X-ray Transient with the shortest orbital period: Suzaku observes one orbit in IGRJ16479-4514
摘要：
食硬X射线源IGR J16479-4514是超巨星快速X射线瞬变源（SFXT），具有最短的轨道周期（3.32天）。这使我们能够在2012年2月对朱雀进行250 k长的X射线观测，覆盖其大部分轨道，包括日食出口。在日食之外，源的光度大约是1 E34 erg/s。X射线谱与6.4 keV的中性铁发射线符合吸收功率定律。在X射线食区之外，柱密度恒定在1 E23 cm-2。在日食期间，它是较低的，与在日食期间由超巨星伴星风散射低X射线发射源一致。在X射线食期间的散射X射线发射被用来直接探测在轨道分离处的伴随风的密度，产生7 E-14 g/cm 3，其转化为风质量损失率与风终极速度的比率Mdot_w/v_terminal = 7 E-17太阳质量/km。假设合理的终极速度在500-3000 km/s范围内，这个比率转化为吸积光度比观测到的高两个数量级。我们的结论是，一个机制，减少吸积率到紧凑的对象是在工作中，可能是由于中子星磁层。
英文摘要：
The eclipsing hard X-ray source IGR J16479-4514 is the Supergiant Fast X-ray Transient (SFXT) with the shortest orbital period (3.32 days). This allowed us to perform a 250 ks long X-ray observation with Suzaku in 2012 February, covering most of its orbit, including the eclipse egress. Outside the eclipse, the source luminosity is around a few 1E34erg/s. The X-ray spectrum can be fit with an absorbed power law together with a neutral iron emission line at 6.4 keV. The column density is constant at 1E23 cm-2 outside the X-ray eclipse. During the eclipse it is lower, consistent with a scattering origin for the low X-ray emission during the eclipse by the supergiant companion wind. The scattered X-ray emission during the X-ray eclipse is used to directly probe the density of the companion wind at the orbital separation, resulting in 7E-14 g/cm3, which translates into a ratio Mdot_w/v_terminal = 7E-17 solar masses/km of the wind mass loss rate to the wind terminal velocity. This ratio, assuming reasonable terminal velocities in the range 500-3000 km/s, translates into an accretion luminosity two orders of magnitude higher than that observed. We conclude that a mechanism reducing the accretion rate onto the compact object is at work, likely due to the neutron star magnetosphere.
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