论文标题
弗拉德多超级 - 埃德丁顿的风力动态
The Wind Dynamics of Super-Eddington Sources in FRADO
论文作者
论文摘要
我们执行非流动力学2.5D模拟，以基于作用于灰尘的磁盘辐射压力来研究材料上方材料的动力学。我们假设一个超固定的基础磁盘，其积聚率是爱丁顿速率的10倍，中央黑洞质量从$ 10^7 $到$ 10^9 m _ {\ odot} $不等。如此高的积聚率是极端来源的特征。我们表明，对于基于Frado模型的辐射驱动机制的高增生器始终导致磁盘表面的大量流出，而失败的风仅在较大的半径下出现。流出速率在很大程度上取决于黑洞的质量，在光厚的能量驱动的解决方案中，大于$ 10^ 8 m _ {\ odot} $的质量的吸积率，但是动量驱动的流出也不会超过超级埃德丁顿的积聚率，因此也不能使迪斯特族的所采用的处代违法。但是，即使在这种情况下，磁盘的流出也意味着强烈的机械反馈。
We perform non-hydrodynamical 2.5D simulations to study the dynamics of material above accretion disk based on the disk radiation pressure acting on dust. We assume a super-accreting underlying disk with the accretion rate of 10 times the Eddington rate with central black hole mass ranging from $10^7$ up to $10^9 M_{\odot}$. Such high accretion rates are characteristic for extreme sources. We show that for high accretors radiatively dust-driving mechanism based on FRADO model always leads to a massive outflow from the disk surface, and the failed wind develops only at larger radii. The outflow rate strongly depends on the black hole mass, and in optically-thick energy-driven solution can exceed the accretion rate for masses larger than $10^ 8 M_{\odot}$ but momentum-driven outflow does not exceed the accretion rate even for super-Eddington accretion, therefore not violating the adopted stationarity of the disk. However, even in this case the outflow from the disk implies a strong mechanical feedback.
