Shock finding on a moving-mesh - II. Hydrodynamic shocks in the Illustris universe

被引：29

作者：

Schaal, Kevin ^{[1
,2
]}

Springel, Volker ^{[1
,2
]}

Pakmor, Ruediger ^{[1
]}

Pfrommer, Christoph ^{[1
]}

Nelson, Dylan ^{[3
]}

Vogelsberger, Mark ^{[4
]}

Genel, Shy ^{[5
]}

Pillepich, Annalisa ^{[6
]}

Sijacki, Debora ^{[7
,8
]}

Hernquist, Lars ^{[6
]}

机构：

[1] Heidelberg Inst Theoret Studies, Schloss Wolfsbrunnenweg 35, D-69118 Heidelberg, Germany

[2] Heidelberg Univ, Zentrum Astron, Astron Recheninst, Monchhofstr 12-14, D-69120 Heidelberg, Germany

[3] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85740 Garching, Germany

[4] MIT, Kavli Inst Astrophys & Space Res, Dept Phys, Cambridge, MA 02139 USA

[5] Columbia Univ, Dept Astron, 550 West 120th St, New York, NY 10027 USA

[6] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA

[7] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England

[8] Univ Cambridge, Kavli Inst Cosmol, Madingley Rd, Cambridge CB3 0HA, England

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2016年 / 461卷 / 04期

基金：

美国国家科学基金会; 欧洲研究理事会;

关键词：

hydrodynamics; shock waves; methods: numerical; galaxies: clusters: general; galaxies: kinematics and dynamics; large-scale structure of Universe; LARGE-SCALE STRUCTURE; SIMULATING COSMIC-RAYS; EXTENDED RADIO-EMISSION; COSMOLOGICAL SIMULATIONS; X-RAY; GALAXY CLUSTERS; STAR-FORMATION; BLACK-HOLES; BOW SHOCK; PARTICLE-ACCELERATION;

D O I：

10.1093/mnras/stw1587

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Hydrodynamical shocks are a manifestation of the non-linearity of the Euler equations and play a fundamental role in cosmological gas dynamics. In this work, we identify and analyse shocks in the Illustris simulation, and contrast the results with those of non-radiative runs. We show that simulations with more comprehensive physical models of galaxy formation pose new challenges for shock finding algorithms due to radiative cooling and star-forming processes, prompting us to develop a number of methodology improvements. We find in Illustris a total shock surface area which is about 1.4 times larger at the present epoch compared to non-radiative runs, and an energy dissipation rate at shocks which is higher by a factor of around 7. Remarkably, shocks with Mach numbers above and below M approximate to 10 contribute about equally to the total dissipation across cosmic time. This is in sharp contrast to non-radiative simulations, and we demonstrate that a large part of the difference arises due to strong black hole radiomode feedback in Illustris. We also provide an overview of the large diversity of shock morphologies, which includes complex networks of halo-internal shocks, shocks on to cosmic sheets, feedback shocks due to black holes and galactic winds, as well as ubiquitous accretion shocks. In high-redshift systems more massive than 10(12) M-circle dot, we discover the existence of a double accretion shock pattern in haloes. They are created when gas streams along filaments without being shocked at the outer accretion shock, but then forms a second, roughly spherical accretion shock further inside.

引用

页码：4441 / 4465

页数：25

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