潮汐瓦解事件中的各向异性风
Anisotropic wind in tidal disruption events
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- Leiden University（莱顿大学）
- University of Wisconsin, Madison（威斯康星大学麦迪逊分校）
- The Hebrew University（希伯来大学）
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中文总结 AI 辅助
本研究通过三维辐射流体动力学模拟，发现潮汐瓦解事件外流呈现各向异性，导致观测角度依赖的光度与谱线特征，并预测其光学/紫外辐射可被LSST和ULTRASAT探测到。
中文摘要 AI 辅助
在未来几年，随着薇拉·鲁宾天文台（g和r波段）以及{\it ULTRASAT}（近紫外）巡天观测的到来，潮汐瓦解事件（TDEs）的数量预计将大幅增加。这些未来的样本有望刻画大质量黑洞质量函数的低端，但现有的中等质量黑洞TDE探测主要局限于X射线波段，其光学/紫外辐射在很大程度上尚未被探索。我们利用RICH代码，对一颗$10^4 M_\odot$黑洞以现实参数发生的TDE进行了三维端到端辐射流体动力学模拟，并提出了对近心点附近耗散产生的外流的时间与角度依赖分析。我们发现外流各向异性产生了依赖观测角度的可观测特征。朝向极区和近心点区域，质量损失率较低，而热光度达到爱丁顿光度的约2至3倍。朝向流方向，性质显示出对纬度的更强依赖：随着视线接近轨道平面，质量损失率增加而热光度降低。这些更致密的区域有利于H$\alpha$和H$\beta$发射。尽管存在这些变化，所有观测方向都表现出共同的光谱演化：初始的软X射线耀发，随后（约$1.25t_{\rm fb}\approx3$天）激波驱动的发射被再处理到紫外和光学波段。尽管我们预测的该TDE的光学/紫外光度对于过去的巡天（如ASAS-SN、ZTF）可能过于暗淡，但它们处于LSST和ULTRASAT的探测能力范围内，对于最亮的观测方向，其探测地平线分别约为790和340 Mpc。
英文摘要
Over the coming years, the number of tidal disruption events (TDEs) is expected to substantially increase with observations from the Vera Rubin Observatory (g and r band) and {\it ULTRASAT} (near UV) wide-field surveys. These future samples have great promise to characterize the bottom end of the massive black hole mass function, but existing detections of intermediate mass black hole TDEs are primarily in X-rays, leaving their optical/UV emission largely unexplored. We present a time- and angle-dependent analysis of the outflow produced by dissipation near pericentre in a three-dimensional end-to-end radiation-hydrodynamics simulation of a TDE by a $10^4 M_\odot$ black hole with realistic parameters, run with the code RICH. We find that outflow anisotropy produces viewing-angle-dependent observables. Towards the poles and the pericentre region, mass-loss rates are low and bolometric luminosities reach $\sim2$--$3$ times the Eddington luminosity. Towards the stream, the properties show a stronger dependence on latitude: the mass-loss rate increases and the bolometric luminosity decreases as the line of sight approaches the orbital plane. These denser regions favour H$α$ and H$β$ emission. Despite these variations, all viewing directions show a common spectral evolution, with an initial soft X-ray flare followed (around $1.25t_{\rm fb}\approx3$~days) by the reprocessing of shock-powered emission into the UV and optical bands. Although the optical/UV luminosities we predict for this TDE are likely too dim for past surveys (e.g. ASAS-SN, ZTF), they are within the detection capabilities of LSST and ULTRASAT to horizons of $\sim 790$ and $\sim 340$ Mpc, respectively, for the brightest viewing directions.
