报告摘要：The formation of jets in black hole accretion systems is a long-standing problem. It has been proposed that a jet can be formed by extracting the rotation energy of the black hole (“BZ-jet”) or the accretion flow (“BP-jet”). But both models are purely dynamical and it is unclear whether they can reproduce the various observations of jets. By performing general relativistic MHD simulations and considering electron acceleration by magnetic reconnection, we have calculated the predicted images by the two models and compared them to observations of the jet in M87, which is best observationally constrained among all jets. We find that the BZ-jet originating from a magnetically arrested disk around a high-spin black hole can well reproduce observations, including jet width and limb-brightening feature, while BP-jet cannot. The physical origin of reconnection is analyzed and found to be likely driven by magnetic eruption in the underlying accretion flow.

主讲人简介：1997年于中国科学技术大学获博士学位，之后在南京大学、马普射电天文研究所、哈佛大学、普渡大学进行博士后研究工作，2005-2023年任中国科学院上海天文台研究员，期间曾任上海天文台学术委员会主任、副台长、中国科学院星系宇宙学重点实验室主任、6163银河线路检测中心-上海天文台联合天体物理中心联合主任等职。2024年起任复旦大学特聘教授、复旦大学天文与天体物理中心主任。兼任6163银河线路检测中心等几所高校的兼职或者讲席教授。曾获得国家杰出青年基金、上海市自然科学牡丹奖、基础物理突破奖等奖项。主要研究方向黑洞吸积与外流理论、活动星系核、星系形成与演化，发表论文200余篇，包括一篇ARA&A，被引用20000余次。在重要国际会议做邀请报告60余次。主持了包括基金委重大等项目，是“黑洞事件视界望远镜”国际合作发起人之一、首届论文工作委员会五名委员之一。