Modeling the inner part of the jet in M87: Confronting jet morphology with theory

被引：17

作者：

Yang, Hai ^{[1
,2
,3
]}

Yuan, Feng ^{[1
,2
,4
,5
]}

Li, Hui ^{[6
]}

Mizuno, Yosuke ^{[3
,7
,8
]}

Guo, Fan ^{[6
]}

Lu, Rusen ^{[1
,9
,10
]}

Ho, Luis C. ^{[11
,12
]}

Lin, Xi ^{[1
,2
]}

Zdziarski, Andrzej A. ^{[13
]}

Wang, Jieshuang ^{[14
]}

机构：

[1] Chinese Acad Sci, Shanghai Astron Observ, 80 Nandan Rd, Shanghai 200030, Peoples R China

[2] Univ Chinese Acad Sci, 19A Yuquan Rd, Beijing 100049, Peoples R China

[3] Shanghai Jiao Tong Univ, Tsung Dao Lee Inst, Shengrong Rd 520, Shanghai 201210, Peoples R China

[4] Fudan Univ, Ctr Astron & Astrophys, Shanghai 200438, Peoples R China

[5] Fudan Univ, Dept Phys, Shanghai 200438, Peoples R China

[6] Los Alamos Natl Lab, Los Alamos, NM 87545 USA

[7] Shanghai Jiao Tong Univ, Sch Phys & Astron, 800 Dongchuan Rd, Shanghai 200240, Peoples R China

[8] Goethe Univ Frankfurt, Inst Theoret Phys, Max von Laue Str 1, D-60438 Frankfurt, Germany

[9] Chinese Acad Sci, Key Lab Radio Astron & Technol, A20 Datun Rd, Beijing 100101, Peoples R China

[10] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany

[11] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China

[12] Peking Univ, Sch Phys, Dept Astron, Beijing 100871, Peoples R China

[13] Polish Acad Sci, Nicolaus Copernicus Astron Ctr, Bartycka 18, PL-00716 Warsaw, Poland

[14] Max Planck Inst Kernphys, Saupfercheckweg 1, D-69117 Heidelberg, Germany

来源：

SCIENCE ADVANCES | 2024年 / 10卷 / 12期

基金：

中国国家自然科学基金;

关键词：

RELATIVISTIC MAGNETOHYDRODYNAMIC SIMULATIONS; BLACK-HOLE; EVENT HORIZON; ACCRETION FLOWS; DISKS; ACCELERATION; ORIGIN; FLARES; ENERGY; DISCS;

D O I：

10.1126/sciadv.adn3544

中图分类号：

O [数理科学和化学]; P [天文学、地球科学]; Q [生物科学]; N [自然科学总论];

学科分类号：

07 ; 0710 ; 09 ;

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.

引用

页数：11

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