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Verfasst von:Treß, Robin G. [VerfasserIn]   i
 Sormani, Mattia C. [VerfasserIn]   i
 Smith, Rowan J. [VerfasserIn]   i
 Glover, Simon [VerfasserIn]   i
 Klessen, Ralf S. [VerfasserIn]   i
 Mac Low, Mordecai-Mark [VerfasserIn]   i
 Clark, Paul C. [VerfasserIn]   i
 Duarte-Cabral, Ana [VerfasserIn]   i
Titel:Simulations of the star-forming molecular gas in an interacting M51-like galaxy
Titelzusatz:cloud population statistics
Verf.angabe:Robin G. Treß, Mattia C. Sormani, Rowan J. Smith, Simon C.O. Glover, Ralf S. Klessen, Mordecai-Mark Mac Low, Paul Clark and Ana Duarte-Cabral
E-Jahr:2021
Jahr:2021 June 12
Umfang:22 S.
Fussnoten:Gesehen am 01.12.2021
Titel Quelle:Enthalten in: Royal Astronomical SocietyMonthly notices of the Royal Astronomical Society
Ort Quelle:Oxford : Oxford Univ. Press, 1827
Jahr Quelle:2021
Band/Heft Quelle:505(2021), 4, Seite 5438-5459
ISSN Quelle:1365-2966
Abstract:To investigate how molecular clouds react to different environmental conditions at a galactic scale, we present a catalogue of giant molecular clouds (GMCs) resolved down to masses of ∼10 M⊙ from a simulation of the entire disc of an interacting M51-like galaxy and a comparable isolated galaxy. Our model includes time-dependent gas chemistry, sink particles for star formation, and supernova feedback, meaning we are not reliant on star formation recipes based on threshold densities and can follow the physics of the cold molecular phase. We extract GMCs from the simulations and analyse their properties. In the disc of our simulated galaxies, spiral arms seem to act merely as snowplows, gathering gas, and clouds without dramatically affecting their properties. In the centre of the galaxy, on the other hand, environmental conditions lead to larger, more massive clouds. While the galaxy interaction has little effect on cloud masses and sizes, it does promote the formation of counter-rotating clouds. We find that the identified clouds seem to be largely gravitationally unbound at first glance, but a closer analysis of the hierarchical structure of the molecular interstellar medium shows that there is a large range of virial parameters with a smooth transition from unbound to mostly bound for the densest structures. The common observation that clouds appear to be virialized entities may therefore be due to CO bright emission highlighting a specific level in this hierarchical binding sequence. The small fraction of gravitationally bound structures found suggests that low galactic star formation efficiencies may be set by the process of cloud formation and initial collapse.
DOI:doi:10.1093/mnras/stab1683
URL:Bitte beachten Sie: Dies ist ein Bibliographieeintrag. Ein Volltextzugriff für Mitglieder der Universität besteht hier nur, falls für die entsprechende Zeitschrift/den entsprechenden Sammelband ein Abonnement besteht oder es sich um einen OpenAccess-Titel handelt.

Volltext: https://doi.org/10.1093/mnras/stab1683
 DOI: https://doi.org/10.1093/mnras/stab1683
Datenträger:Online-Ressource
Sprache:eng
K10plus-PPN:1780012888
Verknüpfungen:→ Zeitschrift

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