Density distribution function of a self-gravitating isothermal turbulent fluid in the context of molecular cloud ensembles: III. Virial analysis
In this work, we apply virial analysis to the model of self-gravitating turbulent cloud ensembles introduced by Donkov & Stefanov in two previous papers, clarifying some aspects of turbulence and extending the model to account not only for supersonic flows but for trans- and subsonic ones as wel...
Gespeichert in:
| Hauptverfasser: | , , , |
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| Dokumenttyp: | Article (Journal) |
| Sprache: | Englisch |
| Veröffentlicht: |
November 2022
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| In: |
Monthly notices of the Royal Astronomical Society
Year: 2022, Jahrgang: 516, Heft: 4, Pages: 5726-5736 |
| ISSN: | 1365-2966 |
| DOI: | 10.1093/mnras/stac2660 |
| Online-Zugang: | Verlag, lizenzpflichtig, Volltext: https://doi.org/10.1093/mnras/stac2660 Verlag, lizenzpflichtig, Volltext: https://academic.oup.com/mnras/article/516/4/5726/6708380 
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| Verfasserangaben: | S Donkov, I.Zh. Stefanov, T.V. Veltchev and R.S. Klessen |
MARC
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| 245 | 1 | 0 | |a Density distribution function of a self-gravitating isothermal turbulent fluid in the context of molecular cloud ensembles |b III. Virial analysis |c S Donkov, I.Zh. Stefanov, T.V. Veltchev and R.S. Klessen |
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| 520 | |a In this work, we apply virial analysis to the model of self-gravitating turbulent cloud ensembles introduced by Donkov & Stefanov in two previous papers, clarifying some aspects of turbulence and extending the model to account not only for supersonic flows but for trans- and subsonic ones as well. Making use of the Eulerian virial theorem at an arbitrary scale, far from the cloud core, we derive an equation for the density profile and solve it in approximate way. The result confirms the solution ϱ(ℓ) = ℓ−2 found in the previous papers. This solution corresponds to three possible configurations for the energy balance. For trans- or subsonic flows, we obtain a balance between the gravitational and thermal energy (Case 1) or between the gravitational, turbulent, and thermal energies (Case 2) while for supersonic flows, the possible balance is between the gravitational and turbulent energy (Case 3). In Cases 1 and 2, the energy of the fluid element can be negative or zero; thus the solution is dynamically stable and shall be long lived. In Case 3, the energy of the fluid element is positive or zero, i.e. the solution is unstable or at best marginally bound. At scales near the core, one cannot neglect the second derivative of the moment of inertia of the gas, which prevents derivation of an analytic equation for the density profile. However, we obtain that gas near the core is not virialized and its state is marginally bound since the energy of the fluid element vanishes. | ||
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