Turbulence and the characteristics of circumstellar discs
We investigate the properties of circumstellar discs (CDs) produced in hydrodynamical simulations of gravoturbulent core collapse considering Kolmogorov and Burger-type turbulence. We report that massive discs are more prevalent in the Kolmogorov regime than for Burger-type turbulence. A significant...
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| Hauptverfasser: | , , , , |
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| Dokumenttyp: | Article (Journal) |
| Sprache: | Englisch |
| Veröffentlicht: |
17 June 2024
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| In: |
Monthly notices of the Royal Astronomical Society
Year: 2024, Jahrgang: 532, Heft: 1, Pages: 763-782 |
| ISSN: | 1365-2966 |
| DOI: | 10.1093/mnras/stae1451 |
| Online-Zugang: | Verlag, kostenfrei, Volltext: https://doi.org/10.1093/mnras/stae1451 Verlag, kostenfrei, Volltext: https://academic.oup.com/mnras/article/532/1/763/7695308 
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| Verfasserangaben: | R. Riaz, D.R.G. Schleicher, S. Vanaverbeke, Ralf S. Klessen and J. Saavedra-Bastidas |
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| 520 | |a We investigate the properties of circumstellar discs (CDs) produced in hydrodynamical simulations of gravoturbulent core collapse considering Kolmogorov and Burger-type turbulence. We report that massive discs are more prevalent in the Kolmogorov regime than for Burger-type turbulence. A significant number of discs are formed with a radius of ∼15 au in both cases. However, the number of extended discs with radii >15 au is significantly larger in case of Kolmogorov turbulence. The two regimes of turbulence, in general, yield disc radii in the ranges of 7−30 au and 13−39 au, respectively. The corresponding ranges of the disc masses are 30.37 MJup−0.92 M and 2.09 MJup−0.13 M , respectively. Moreover, the ratio Mdisc/Mstar is higher in models of Kolmogorov-type turbulence than in models of Burgers-type turbulence. We do not find any correlation between Rdisc and Mdisc over the explored range of initial temperatures (8−14 K) and the type of turbulence. Also, for these initial thermal variations, the turbulent CD structures do not exhibit signs of turbulent diffusion. Nonetheless, both sub- and supersonic velocity dispersions cause variations in the specific angular momentum of infalling gas, especially for CDs with radii ∼ 16−21 au. The radial profiles of CDs do not correlate with the initial conditions. | ||
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