通过Rayleigh-Taylor不稳定性吸积到磁化星：全球三维模拟
Accretion to Magnetized Stars through the Rayleigh-Taylor Instability: Global Three-Dimensional Simulations
摘要：
本文给出了吸积盘-磁层边界MHD不稳定性的三维模拟结果。这种不稳定性是瑞利-泰勒不稳定性，并在相当宽的吸积率、恒星自转率和磁场范围内发展。它以细长的等离子体舌头的形式出现，这些舌头穿过赤道平面的磁层。在内盘动力学时间尺度上，舌的形状和数量随时间变化。与漏斗流不同，漏斗流主要在极地地区沉积物质，而舌状流则在更靠近恒星赤道的地方沉积物质。这种不稳定性出现在恒星自转轴和磁轴之间相对较小的错位角$Θ\lesssim30^\circ$时，并且与较高的吸积率有关。通过不稳定性吸积过程中的热点和光变曲线通常比稳定吸积过程中更混乱。吸积的不稳定状态可能对吸积系统的准周期振荡和间歇性脉动以及行星迁移产生影响。
英文摘要：
We present results of 3D simulations of MHD instabilities at the accretion disk-magnetosphere boundary. The instability is Rayleigh-Taylor, and develops for a fairly broad range of accretion rates and stellar rotation rates and magnetic fields. It manifests itself in the form of tall, thin tongues of plasma that penetrate the magnetosphere in the equatorial plane. The shape and number of the tongues changes with time on the inner-disk dynamical timescale. In contrast with funnel flows, which deposit matter mainly in the polar region, the tongues deposit matter much closer to the stellar equator. The instability appears for relatively small misalignment angles, $Θ\lesssim30^\circ$, between the star's rotation and magnetic axes, and is associated with higher accretion rates. The hot spots and light curves during accretion through instability are generally much more chaotic than during stable accretion. The unstable state of accretion has possible implications for quasi-periodic oscillations and intermittent pulsations from accreting systems, as well as planet migration.
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