報告摘要：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.

主講人簡介：1997年于中國科學技術大學獲博士學位，之後在南京大學、馬普射電天文研究所、哈佛大學、普渡大學進行博士後研究工作，2005-2023年任中國科學院上海天文台研究員，期間曾任上海天文台學術委員會主任、副台長、中國科學院星系宇宙學重點實驗室主任、beat365-上海天文台聯合天體物理中心聯合主任等職。2024年起任複旦大學特聘教授、複旦大學天文與天體物理中心主任。兼任beat365等幾所高校的兼職或者講席教授。曾獲得國家傑出青年基金、上海市自然科學牡丹獎、基礎物理突破獎等獎項。主要研究方向黑洞吸積與外流理論、活動星系核、星系形成與演化，發表論文200餘篇，包括一篇ARA&A，被引用20000餘次。在重要國際會議做邀請報告60餘次。主持了包括基金委重大等項目，是“黑洞事件視界望遠鏡”國際合作發起人之一、首屆論文工作委員會五名委員之一。