论文标题
用h $α$光谱划分X射线瞬态Maxi J1659-152中的黑洞质量
Delimiting the black hole mass in the X-ray transient MAXI J1659-152 with H$α$ spectroscopy
论文作者
论文摘要
Maxi J1659-152是2.4 h轨道周期X射线浸入瞬态黑洞候选者。我们介绍了其$ i \ of23 $ quiescent对应物的光谱，在其中我们检测到h $α$的排放，全宽度为fall tidth，为$ 3200 \ $ 3200 \ pm 300 $ km s $ s $^{ - 1} $。在静态X射线瞬变中应用H $α$ FWHM和径向速度半振幅之间的相关性，我们得出$ k_2 = 750 \ pm 80 $ km s $^{ - 1} $。轨道周期和$ k_2 $导致质量功能$ 4.4 \ pm1.4〜m {_ \ odot} $（1 $σ$）。紧凑对象质量比和二进制倾斜度的供体可能在$ q = {m_2}/{m_1} = 0.02-0.07 $和$ i = 70 {^\ circ} -80 {^\ circ} $。这些约束意味着紧凑型物体质量为$ 3.3 \ Lessim m_1（m_ \ odot）\ Lessim 7.5 $的68％置信度间隔，确认其黑洞性质。将这些准动力学限制与X射线数据建模的质量估计进行了比较，并讨论了所有差异。我们回顾了2010- 2011年爆发期间收集的光谱和时间序列光度法的特性。我们将高核活动发作和2011年重新布置事件发作后不久，将其解释为起源盘。这些签名与超级烟一致，2011年调制的分数超过$ <0.6 \％$（3 $σ$）。我们建议，由于圆盘外区域的掩星，无法通过中央X射线源对供体进行直接照射。我们认为，圆盘屏蔽会大大削弱供体星对具有$ Q \ lyssim0.07 $的系统的光学变异性的贡献，其中包括Neutron Star Ulta-Cromcact X射线二进制文件。
MAXI J1659-152 is a 2.4 h orbital period X-ray dipping transient black hole candidate. We present spectroscopy of its $I\approx23$ quiescent counterpart where we detect H$α$ emission with full-width at half-maximum (FWHM) of $3200 \pm 300$ km s$^{-1}$. Applying the correlation between the H$α$ FWHM and radial velocity semi-amplitude of the donor star for quiescent X-ray transients, we derive $K_2 = 750 \pm 80$ km s$^{-1}$. The orbital period and $K_2$ lead to a mass function of $4.4\pm1.4~M{_\odot}$ (1$σ$). The donor to compact object mass ratio and binary inclination are likely in the range $q={M_2}/{M_1} = 0.02-0.07$ and $i=70{^\circ}-80{^\circ}$. These constraints imply a 68% confidence level interval for the compact object mass of $3.3 \lesssim M_1(M_\odot) \lesssim 7.5$, confirming its black hole nature. These quasi-dynamical limits are compared to mass estimates from modelling of X-ray data and any discrepancies are discussed. We review the properties of optical spectroscopy and time-series photometry collected during the 2010-2011 outburst. We interpret the apparent modulations found soon after the onset of high-accretion activity and during the 2011 rebrightening event as originating in the accretion disc. These have signatures consistent with superhumps, with the 2011 modulation having a fractional period excess $< 0.6\%$ (3$σ$). We propose that direct irradiation of the donor by the central X-ray source was not possible due to its occultation by the disc outer regions. We argue that disc shielding significantly weakens the donor star contribution to the optical variability in systems with $q\lesssim0.07$, including neutron star ultra-compact X-ray binaries.
