Alignment of Magnetized Accretion Disks and Relativistic Jets with Spinning Black Holes

被引：159

作者：

McKinney, Jonathan C. ^{[1
,2
,3
]}

Tchekhovskoy, Alexander ^{[4
]}

Blandford, Roger D. ^{[1
]}

机构：

[1] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94309 USA

[2] Univ Maryland, Dept Phys, College Pk, MD 20742 USA

[3] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA

[4] Princeton Univ, Ctr Theoret Sci, Princeton, NJ 08544 USA

来源：

SCIENCE | 2013年 / 339卷 / 6115期

关键词：

SAGITTARIUS-A-ASTERISK; SIMULATIONS; ENERGY; MODEL; EXTRACTION; EMISSION; M87;

D O I：

10.1126/science.1230811

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：

Accreting black holes (BHs) produce intense radiation and powerful relativistic jets, which are affected by the BH's spin magnitude and direction. Although thin disks might align with the BH spin axis via the Bardeen-Petterson effect, this does not apply to jet systems with thick disks. We used fully three-dimensional general relativistic magnetohydrodynamical simulations to study accreting BHs with various spin vectors and disk thicknesses and with magnetic flux reaching saturation. Our simulations reveal a "magneto-spin alignment" mechanism that causes magnetized disks and jets to align with the BH spin near BHs and to reorient with the outer disk farther away. This mechanism has implications for the evolution of BH mass and spin, BH feedback on host galaxies, and resolved BH images for the accreting BHs in SgrA* and M87.

引用

页码：49 / 52

页数：4

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