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Verfasst von:Seifried, Daniel Jürgen [VerfasserIn]   i
 Girichidis, Philipp [VerfasserIn]   i
 Klessen, Ralf S. [VerfasserIn]   i
 Glover, Simon [VerfasserIn]   i
Titel:SILCC-Zoom
Titelzusatz:the dynamical and chemical evolution of molecular clouds
Verf.angabe:D. Seifried, S. Walch, P. Girichidis, T. Naab, R. Wünsch, R.S. Klessen, S.C.O. Glover, T. Peters and P. Clark
Umfang:22 S.
Fussnoten:Advance Access publication 2017 September 11 ; Gesehen am 29.06.2018
Titel Quelle:Enthalten in: Royal Astronomical Society: Monthly notices of the Royal Astronomical Society
Jahr Quelle:2017
Band/Heft Quelle:472(2017), 4, S. 4797-4818
ISSN Quelle:1365-2966
Abstract:We present 3D "zoom-in" simulations of the formation of two molecular clouds out of the galactic interstellar medium. We model the clouds - identified from the SILCC simulations - with a resolution of up to 0.06 pc using adaptive mesh refinement in combination with a chemical network to follow heating, cooling, and the formation of H$_2$ and CO including (self-) shielding. The two clouds are assembled within a few million years with mass growth rates of up to $\sim$ 10$^{-2}$ M$_\mathrm{sun}$ yr$^{-1}$ and final masses of $\sim$ 50 000 M$_\mathrm{sun}$. A spatial resolution of $\lesssim$ 0.1 pc is required for convergence with respect to the mass, velocity dispersion, and chemical abundances of the clouds, although these properties also depend on the cloud definition such as based on density thresholds, H$_2$ or CO mass fraction. To avoid grid artefacts, the progressive increase of resolution has to occur within the free-fall time of the densest structures (1 - 1.5 Myr) and $gtrsim$ 200 time steps should be spent on each refinement level before the resolution is progressively increased further. This avoids the formation of spurious, large-scale, rotating clumps from unresolved turbulent flows. While CO is a good tracer for the evolution of dense gas with number densities $n \geq$ 300 cm$^{-3}$, H$_2$ is also found for $n \lesssim 30$ cm$^{-3}$ due to turbulent mixing and becomes dominant at column densities around 30 - 50 M$_\mathrm{sun}$ pc$^{-2}$. The CO-to-H$_2$ ratio steadily increases within the first 2 Myr whereas $X_\mathrm{CO}\simeq$ 1 - 4 $\times$ 10$^{20}$ cm$^{-2}$ (K km s$^{-1}$)$^{-1}$ is approximately constant since the CO(1-0) line quickly becomes optically thick.
DOI:doi:10.1093/mnras/stx2343
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.

Kostenfrei: Verlag: http://dx.doi.org/10.1093/mnras/stx2343
 Kostenfrei: Verlag: http://arxiv.org/abs/1704.06487
 DOI: https://doi.org/10.1093/mnras/stx2343
Datenträger:Online-Ressource
Sprache:eng
K10plus-PPN:1577064437
Verknüpfungen:→ Zeitschrift

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