Universität zu Köln

Walch, S., Girichidis, P., Naab, T., Gatto, A., Glover, S. C. O., Wuensch, R., Klessen, R. S., Clark, P. C., Peters, T., Derigs, D. and Baczynski, C. (2015). The SILCC (SImulating the LifeCycle of molecular Clouds) project - I. Chemical evolution of the supernova-driven ISM. Mon. Not. Roy. Astron. Soc., 454 (1). S. 238 - 269. OXFORD: OXFORD UNIV PRESS. ISSN 1365-2966

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Abstract

The SILCC (SImulating the Life-Cycle of molecular Clouds) project aims to self-consistently understand the small-scale structure of the interstellar medium (ISM) and its link to galaxy evolution. We simulate the evolution of the multiphase ISM in a (500 pc)(2) x +/-5 kpc region of a galactic disc, with a gas surface density of Sigma(GAS) = 10 M-circle dot pc(-2). The FLASH 4 simulations include an external potential, self-gravity, magnetic fields, heating and radiative cooling, time-dependent chemistry of H-2 and CO considering (self-) shielding, and supernova (SN) feedback but omit shear due to galactic rotation. We explore SN explosions at different rates in high-density regions (peak), in random locations with a Gaussian distribution in the vertical direction (random), in a combination of both (mixed), or clustered in space and time (clus/clus2). Only models with self-gravity and a significant fraction of SNe that explode in low-density gas are in agreement with observations. Without self-gravity and in models with peak driving the formation of H-2 is strongly suppressed. For decreasing SN rates, the H-2 mass fraction increases significantly from <10 per cent for high SN rates, i.e. 0.5 dex above Kennicutt-Schmidt, to 70-85 per cent for low SN rates, i.e. 0.5 dex below KS. For an intermediate SN rate, clustered driving results in slightly more H-2 than random driving due to the more coherent compression of the gas in larger bubbles. Magnetic fields have little impact on the final disc structure but affect the dense gas (n greater than or similar to 10 cm(-3)) and delay H-2 formation. Most of the volume is filled with hot gas (similar to 80 per cent within +/-150 pc). For all but peak driving a vertically expanding warm component of atomic hydrogen indicates a fountain flow. We highlight that individual chemical species populate different ISM phases and cannot be accurately modelled with temperature-/density-based phase cut-offs.

Item Type:	Journal Article
Creators:	Creators Email ORCID ORCID Put Code Walch, S. UNSPECIFIED UNSPECIFIED UNSPECIFIED Girichidis, P. UNSPECIFIED UNSPECIFIED UNSPECIFIED Naab, T. UNSPECIFIED UNSPECIFIED UNSPECIFIED Gatto, A. UNSPECIFIED UNSPECIFIED UNSPECIFIED Glover, S. C. O. UNSPECIFIED UNSPECIFIED UNSPECIFIED Wuensch, R. UNSPECIFIED UNSPECIFIED UNSPECIFIED Klessen, R. S. UNSPECIFIED UNSPECIFIED UNSPECIFIED Clark, P. C. UNSPECIFIED UNSPECIFIED UNSPECIFIED Peters, T. UNSPECIFIED UNSPECIFIED UNSPECIFIED Derigs, D. UNSPECIFIED UNSPECIFIED UNSPECIFIED Baczynski, C. UNSPECIFIED UNSPECIFIED UNSPECIFIED
URN:	urn:nbn:de:hbz:38-386843
DOI:	10.1093/mnras/stv1975
Journal or Publication Title:	Mon. Not. Roy. Astron. Soc.
Volume:	454
Number:	1
Page Range:	S. 238 - 269
Date:	2015
Publisher:	OXFORD UNIV PRESS
Place of Publication:	OXFORD
ISSN:	1365-2966
Language:	English
Faculty:	Unspecified
Divisions:	Unspecified
Subjects:	no entry
Uncontrolled Keywords:	Keywords Language STAR-FORMING GALAXIES; MULTIPHASE GALACTIC DISKS; THERMAL/DYNAMICAL EQUILIBRIUM-MODEL; TURBULENT INTERSTELLAR-MEDIUM; NEUTRAL ATOMIC PHASES; INITIAL MASS FUNCTION; STELLAR FEEDBACK; FORMATION RATES; MAGNETIC-FIELD; HYDRODYNAMIC SIMULATIONS Multiple languages Astronomy & Astrophysics Multiple languages
URI:	http://kups.ub.uni-koeln.de/id/eprint/38684