Universität zu Köln

Peters, Thomas, Naab, Thorsten ORCID: 0000-0002-7314-2558, Walch, Stefanie, Glover, Simon C. O., Girichidis, Philipp ORCID: 0000-0002-9300-9914, Pellegrini, Eric, Klessen, Ralf S., Wunsch, Richard ORCID: 0000-0003-1848-8967, Gatto, Andrea and Baczynski, Christian (2017). The SILCC project - IV. Impact of dissociating and ionizing radiation on the interstellar medium and Ha emission as a tracer of the star formation rate. Mon. Not. Roy. Astron. Soc., 466 (3). S. 3293 - 3309. OXFORD: OXFORD UNIV PRESS. ISSN 1365-2966

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Abstract

We present three-dimensional radiation-hydrodynamical simulations of the impact of stellar winds, photoelectric heating, photodissociating and photoionizing radiation, and supernovae on the chemical composition and star formation in a stratified disc model. This is followed by a sink-based model for star clusters with populations of individual massive stars. Stellar winds and ionizing radiation regulate the star formation rate at a factor of similar to 10 below the simulation with only supernova feedback due to their immediate impact on the ambient interstellar medium after star formation. Ionizing radiation (with winds and supernovae) significantly reduces the ambient densities for most supernova explosions to. 10-25 g cm(-3), compared to 10-23g cm(-3) for the model with only winds and supernovae. Radiation from massive stars reduces the amount of molecular hydrogen and increases the neutral hydrogen mass and volume filling fraction. Only this model results in a molecular gas depletion time-scale of 2 Gyr and shows the best agreement with observations. In the radiative models, the Ha emission is dominated by radiative recombination as opposed to collisional excitation (the dominant emission in non-radiative models), which only contributes similar to 1-10 per cent to the total Ha emission. Individual massive stars (M >= 30M(circle dot)) with short lifetimes are responsible for significant fluctuations in the Ha luminosities. The corresponding inferred star formation rates can underestimate the true instantaneous star formation rate by a factor of similar to 10.

Item Type:	Journal Article
Creators:	Creators Email ORCID ORCID Put Code Peters, Thomas UNSPECIFIED UNSPECIFIED UNSPECIFIED Naab, Thorsten UNSPECIFIED orcid.org/0000-0002-7314-2558 UNSPECIFIED Walch, Stefanie UNSPECIFIED UNSPECIFIED UNSPECIFIED Glover, Simon C. O. UNSPECIFIED UNSPECIFIED UNSPECIFIED Girichidis, Philipp UNSPECIFIED orcid.org/0000-0002-9300-9914 UNSPECIFIED Pellegrini, Eric UNSPECIFIED UNSPECIFIED UNSPECIFIED Klessen, Ralf S. UNSPECIFIED UNSPECIFIED UNSPECIFIED Wunsch, Richard UNSPECIFIED orcid.org/0000-0003-1848-8967 UNSPECIFIED Gatto, Andrea UNSPECIFIED UNSPECIFIED UNSPECIFIED Baczynski, Christian UNSPECIFIED UNSPECIFIED UNSPECIFIED
URN:	urn:nbn:de:hbz:38-235378
DOI:	10.1093/mnras/stw3216
Journal or Publication Title:	Mon. Not. Roy. Astron. Soc.
Volume:	466
Number:	3
Page Range:	S. 3293 - 3309
Date:	2017
Publisher:	OXFORD UNIV PRESS
Place of Publication:	OXFORD
ISSN:	1365-2966
Language:	English
Faculty:	Unspecified
Divisions:	Unspecified
Subjects:	no entry
Uncontrolled Keywords:	Keywords Language FORMATION RATE INDICATORS; SUPERNOVA-DRIVEN ISM; MOLECULAR CLOUDS; FORMING GALAXIES; MASSIVE STAR; INITIAL CONDITIONS; NEARBY GALAXIES; GALACTIC HALO; MILKY-WAY; GAS Multiple languages Astronomy & Astrophysics Multiple languages
Refereed:	Yes
URI:	http://kups.ub.uni-koeln.de/id/eprint/23537