Propagation of weak shocks in cool-core galaxy clusters in two-temperature magnetohydrodynamics with anisotropic thermal conduction

被引：2

作者：

Komarov, S. ^{[1
]}

Reynolds, C. ^{[1
]}

Churazov, E. ^{[2
,3
]}

机构：

[1] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 OHA, England

[2] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany

[3] Space Res Inst IKI, Profsouznaya 84-32, Moscow 117997, Russia

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2020年 / 497卷 / 02期

基金：

俄罗斯科学基金会; 英国科学技术设施理事会; 欧洲研究理事会;

关键词：

conduction; shock waves; galaxies: clusters: intracluster medium; SOUND-WAVES; PERSEUS CLUSTER; TRANSPORT; TURBULENCE; FEEDBACK; BUBBLES; GAS;

D O I：

10.1093/mnras/staa1986

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We investigate how different magnetohydrodynamic models of propagation of a weak (Mach number similar to 1.2) shock in the core of a galaxy cluster affect its observational appearance, using the Perseus cluster as our fiducial model. In particular, we study how thermal conduction, both isotropic and anisotropic, and ion-electron temperature equilibration modify a weak shock. Strong thermal conduction is expected to produce an electron temperature precursor. Less prominent pressure and density precursors are formed as well. A longer equilibration time largely reduces the density precursor but does not change the electron temperature precursor much. When thermal conduction becomes anisotropic, the intracluster magnetic field imprints its characteristic spatial scale on the distortions of the shock induced by heat fluxes.

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页码：1434 / 1442

页数：9