Multiple power-law tails in the density and column-density distribution in contracting star-forming clumps
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2024
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| author | Veltchev, Todor V. Girichidis, Philipp Marinkova, Lyubov Donkov, Sava Stanchev, Orlin Klessen, Ralf S. |
| author_facet | Veltchev, Todor V. Girichidis, Philipp Marinkova, Lyubov Donkov, Sava Stanchev, Orlin Klessen, Ralf S. |
| contents | We present a numerical study of the evolution of power-law tails (PLTs) in the (column-)density distributions ($N$-PDF, $ρ$-PDF) in contracting star-forming clumps in primordial gas, without and with some initial rotational and/or turbulent support. In all considered runs multiple PLTs emerge shortly after the formation of the first protostar. The first PLT (PLT 1) in the $ρ$-PDF is a stable feature with slope $q_1\simeq -1.3$ which corresponds -- under the condition of preserved spherical symmetry -- to the outer envelope of the protostellar object with density profile $ρ\propto l^{-2}$ in the classical Larson-Penston collapse model, where $l$ is the radius. The second PLT (PLT 2) in the $ρ$-PDF is stable in the pure-infall runs but fluctuates significantly in the runs with initial support against gravity as dozens of protostars form and their mutual tidal forces change the density structure. Its mean slope, $\langle q_2\rangle\simeq -2$, corresponds to a density profile of $ρ\propto l^{-3/2}$ which describes a core in free fall in the classical Larson-Penston collapse model or an attractor solution at scales with dominating protostellar gravity. PLT 1 and PLT 2 in the $N$-PDFs are generally consistent with the observational data of Galactic low-mass star-forming regions from {\it Herschel} data. In the runs with initial support against gravity a third PLT (PLT~3) in the $ρ$-PDFs appears simultaneously with or after the emergence of PLT 2. It is very shallow, with mean slope of $\langle q_3\rangle\simeq -1$, and is associated with the formation of thin protostellar accretion disks. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2401_02148 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Multiple power-law tails in the density and column-density distribution in contracting star-forming clumps Veltchev, Todor V. Girichidis, Philipp Marinkova, Lyubov Donkov, Sava Stanchev, Orlin Klessen, Ralf S. Astrophysics of Galaxies We present a numerical study of the evolution of power-law tails (PLTs) in the (column-)density distributions ($N$-PDF, $ρ$-PDF) in contracting star-forming clumps in primordial gas, without and with some initial rotational and/or turbulent support. In all considered runs multiple PLTs emerge shortly after the formation of the first protostar. The first PLT (PLT 1) in the $ρ$-PDF is a stable feature with slope $q_1\simeq -1.3$ which corresponds -- under the condition of preserved spherical symmetry -- to the outer envelope of the protostellar object with density profile $ρ\propto l^{-2}$ in the classical Larson-Penston collapse model, where $l$ is the radius. The second PLT (PLT 2) in the $ρ$-PDF is stable in the pure-infall runs but fluctuates significantly in the runs with initial support against gravity as dozens of protostars form and their mutual tidal forces change the density structure. Its mean slope, $\langle q_2\rangle\simeq -2$, corresponds to a density profile of $ρ\propto l^{-3/2}$ which describes a core in free fall in the classical Larson-Penston collapse model or an attractor solution at scales with dominating protostellar gravity. PLT 1 and PLT 2 in the $N$-PDFs are generally consistent with the observational data of Galactic low-mass star-forming regions from {\it Herschel} data. In the runs with initial support against gravity a third PLT (PLT~3) in the $ρ$-PDFs appears simultaneously with or after the emergence of PLT 2. It is very shallow, with mean slope of $\langle q_3\rangle\simeq -1$, and is associated with the formation of thin protostellar accretion disks. |
| title | Multiple power-law tails in the density and column-density distribution in contracting star-forming clumps |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2401.02148 |