物理
喷射(流体)
天体物理喷流
增值(金融)
磁流体驱动
天体物理学
黑洞(网络)
辐射传输
准直光
旋转(数学)
磁流体力学
机械
磁场
活动星系核
光学
几何学
银河系
计算机科学
计算机网络
激光器
路由协议
布线(电子设计自动化)
数学
量子力学
链路状态路由协议
作者
Hai Yang,Feng Yuan,Hui Li,Yosuke Mizuno,Fan Guo,Ru-Sen Lu,Luis C. Ho,Xi Lin,A. A. Zdziarski,J. S. Wang
出处
期刊:Science Advances
[American Association for the Advancement of Science (AAAS)]
日期:2024-03-22
卷期号:10 (12)
被引量:12
标识
DOI:10.1126/sciadv.adn3544
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 (“disk-jet”). While both models can produce collimated relativistic outflows, neither has successfully explained the observed jet morphology. By using general relativistic magnetohydrodynamic simulations and considering nonthermal electrons accelerated by magnetic reconnection that is likely driven by magnetic eruption in the underlying accretion flow, we obtain images by radiative transfer calculations and compared them to millimeter observations of the jet in M87. We find that the BZ-jet originating from a magnetically arrested disk around a high-spin black hole can well reproduce the jet morphology, including its width and limb-brightening feature.
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