论文标题
快速旋转的中间质量黑洞3xmm J150052.0+015452
The Rapidly Spinning Intermediate-Mass Black Hole 3XMM J150052.0+015452
论文作者
论文摘要
被黑洞潮汐破坏的恒星可以形成具有超级伊德丁顿质量增生率的积聚盘。内光盘产生的X射线排放可在黑洞质量$ m_ \ bullet $和无量纲旋转参数$ a_ \ bullet $上限制。先前的研究表明，负责潮汐破坏事件的$ m_ \ bullet $ 3xmm J150052.0+015452（以下简称J150052）为$ \ sim $ 10 $ 10 $^{5} m _ {\ odot} $拟合多个上述XMM-Newton和Chandra X射线光谱在源长期衰减中获得的拟合，我们最新的Slim积分盘模型给出了$ M_ \ bullet = 2.0^{+1.0} _ { - 0.3} _ { - 0.3} \ times10^\ times10^{5} {5} m _ {5} m _ {\ odot} $ 0. 84.1％的置信下限）。 2008 - 2014年之间获得的光谱要比2014年之后的光谱要难得多，这种演变可以通过包括电晕对早期光谱的反向弹药的影响来很好地解释。当源积聚率是超级 - 埃德丁顿时，就存在电晕，而没有证据表明其在2014年以后获得的数据效果，当时质量积聚率在Eddington-limit附近。基于我们的光谱研究，我们推断出电晕在光学厚和温暖（$ kt_e = 2.3^{+2.7} _ { - 0.8} $ kev）。我们的J150052的质量和自旋测量确认为IMBH，并指向快速，接近极端的自旋。这些$ m_ \ bullet $和$ a_ \ bullet $ values排除了向量玻色子和质量的轴$ \ sim10^{ - 16} $ ev。
A star tidally disrupted by a black hole can form an accretion disc with a super-Eddington mass accretion rate; the X-ray emission produced by the inner disc provides constraints on the black hole mass $M_\bullet$ and dimensionless spin parameter $a_\bullet$. Previous studies have suggested that the $M_\bullet$ responsible for the tidal disruption event 3XMM J150052.0+015452 (hereafter J150052) is $\sim$10$^{5} M_{\odot}$, in the intermediate black hole (IMBH) regime. Fitting multi-epoch XMM-Newton and Chandra X-ray spectra obtained after 2008 during the source's decade-long decay, with our latest slim accretion disc model gives $M_\bullet = 2.0^{+1.0}_{-0.3}\times10^{5} M_{\odot}$ (at 68% confidence) and $a_\bullet > 0.97$ (a 84.1% confidence lower limit). The spectra obtained between 2008-2014 are significantly harder than those after 2014, an evolution that can be well explained by including the effects of inverse-Comptonisation by a corona on the early-time spectra. The corona is present when the source accretion rate is super-Eddington, while there is no evidence for its effect in data obtained after 2014, when the mass accretion rate is around the Eddington-limit. Based on our spectral study, we infer that the corona is optically thick and warm ($kT_e=2.3^{+2.7}_{-0.8}$ keV). Our mass and spin measurements of J150052 confirm it as an IMBH and point to a rapid, near extremal, spin. These $M_\bullet$ and $a_\bullet$ values rule out both vector bosons and axions of masses $\sim10^{-16}$ eV.
