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Clumps and triggered star formation in ionized molecular clouds
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SYSNO ASEP 0423674 Document Type J - Journal Article R&D Document Type Journal Article Subsidiary J Článek ve WOS Title Clumps and triggered star formation in ionized molecular clouds Author(s) Walch, S. (DE)
Whitworth, A. (GB)
Bisbas, T. (GB)
Wünsch, Richard (ASU-R) RID, ORCID
Hubber, D.A. (GB)Source Title Monthly Notices of the Royal Astronomical Society. - : Oxford University Press - ISSN 0035-8711
Roč. 435, č. 2 (2013), s. 917-927Number of pages 11 s. Language eng - English Country GB - United Kingdom Keywords hydrodynamics ; stars formation ; ISM bubbles Subject RIV BN - Astronomy, Celestial Mechanics, Astrophysics R&D Projects GAP209/12/1795 GA ČR - Czech Science Foundation (CSF) Institutional support ASU-R - RVO:67985815 UT WOS 000325264600003 DOI 10.1093/mnras/stt1115 Annotation Infrared shells and bubbles are ubiquitous in the Galaxy and can generally be associated with H II regions formed around young, massive stars. In this paper, we use high-resolution 3D SPH simulations to explore the effect of a single O7 star emitting photons at 10(49) s(-1) and located at the centre of a molecular cloud with mass 10(4) M-circle dot and radius 6.4 pc; the internal structure of the cloud is characterized by its fractal dimension, D (with 2.0 <= D <= 2.8), and the variance of its (lognormal) density distribution, sigma(2)(O) (with 0.36 <= sigma(2)(O) <= 1.42). Our study focuses on the morphology of the swept-up cold gas and the distribution and statistics of the resulting star formation. If the fractal dimension is low, the border of the H II region is dominated by extended shell-like structures, and these break up into a small number of massive high-density clumps which then spawn star clusters; star formation occurs relatively quickly, and delivers somewhat higher stellar masses. Workplace Astronomical Institute Contact Radka Svašková, bibl@asu.cas.cz, Tel.: 323 620 326 Year of Publishing 2014
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