The structure of H I in galactic discs: simulations versus observations

被引：12

作者：

Acreman, David M. ^{[1
]}

Dobbs, Clare L. ^{[1
,2
,3
]}

Brunt, Christopher M. ^{[1
]}

Douglas, Kevin A. ^{[4
]}

机构：

[1] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England

[2] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany

[3] Univ Sternwarte Munchen, D-81679 Munich, Germany

[4] Arecibo Observ NAIC, Arecibo, PR 00612 USA

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2012年 / 422卷 / 01期

基金：

欧洲研究理事会;

关键词：

methods: numerical; surveys; ISM: atoms; ISM: structure; SMOOTHED PARTICLE HYDRODYNAMICS; NARROW SELF-ABSORPTION; PLANE SURVEY; INTERSTELLAR-MEDIUM; MOLECULAR CLOUDS; STAR-FORMATION; SPIRAL SHOCKS; MILKY-WAY; PHOTODISSOCIATION REGIONS; SUPERNOVA-REMNANTS;

D O I：

10.1111/j.1365-2966.2012.20599.x

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We generate synthetic H I Galactic plane surveys from spiral galaxy simulations which include stellar feedback processes. Compared to a model without feedback we find an increased scale height of H I emission (in better agreement with real observations) and more realistic spatial structure (including supernova blown bubbles). The synthetic data show H I self-absorption with a morphology similar to that seen in observations. The density and temperature of the material responsible for H I self-absorption is consistent with observationally determined values, and is found to be only weakly dependent on absorption strength and star formation efficiency.

引用

页码：241 / 251

页数：11

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