潮汐瓦解事件中的喷射流发射：磁流平流与等离子体负载

本文探讨了潮汐瓦解事件中相对论性喷射的形成机制。研究提出，由恒星瓦解产生的超爱丁顿吸积流可将预存的磁流输送至黑洞附近，进而通过磁重联与粒子对产生过程驱动喷射流。

arXiv:2608.14258v1 Announce Type: new Abstract: A tidal disruption event (TDE) occurs when a star approaches a black hole (BH) and is disrupted by its tidal forces. Although several hundred TDEs have been identified to date, only a small fraction are accompanied by relativistic jets. These jets are thought to be Poynting-flux-dominated outflows powered by the Blandford--Znajek (BZ) mechanism. However, the origin of the magnetic flux and plasma needed to power BZ jets remain unclear. In this Letter, we propose a scenario in which magnetic flux is initially stored in a pre-existing low-Eddington accretion disk around BH, and is subsequently advected toward the BH by the super-Eddington accretion flow formed after the stellar disruption. We show that stars with low densities, such as red giants, can supply sufficient magnetic flux to power a BZ jet. Once sufficient magnetic flux accumulates near the BH, an equatorial current sheet forms where magnetic reconnection produces high-energy gamma rays. We find that photon--photon pair production by these gamma rays supplies the BH magnetosphere with sufficient plasma to launch and sustain a BZ jet. We further show that this mechanism simultaneously provides enough radiating particles to account for the observed prompt emission.