2018MNRAS.474..400A


C.D.S. - SIMBAD4 rel 1.7 - 2021.04.14CEST13:35:22

2018MNRAS.474..400A - Mon. Not. R. Astron. Soc., 474, 400-410 (2018/February-2)

The effect of magnetic fields and ambipolar diffusion on the column density probability distribution function in molecular clouds.

AUDDY S., BASU S. and KUDOH T.

Abstract (from CDS):

Simulations generally show that non-self-gravitating clouds have a lognormal column density (Σ) probability distribution function (PDF), while self-gravitating clouds with active star formation develop a distinct power-law tail at high column density. Although the growth of the power-law can be attributed to gravitational contraction leading to the formation of condensed cores, it is often debated if an observed lognormal shape is a direct consequence of supersonic turbulence alone, or even if it is really observed in molecular clouds. In this paper we run three-dimensional magnetohydrodynamic simulations including ambipolar diffusion with different initial conditions to see the effect of strong magnetic fields and non-linear initial velocity perturbations on the evolution of the column density PDFs. Our simulations show that column density PDFs of clouds with supercritical mass-to-flux ratio, with either linear perturbations or non-linear turbulence, quickly develop a power-law tail such that dN/dlog Σ ∝ Σ–α with index α ≃ 2. Interestingly, clouds with subcritical mass-to-flux ratio also proceed directly to a power-law PDF, but with a much steeper index α ≃ 4. This is a result of gravitationally driven ambipolar diffusion. However, for non-linear perturbations with a turbulent spectrum (vk2 ∝k–4), the column density PDFs of subcritical clouds do retain a lognormal shape for a major part of the cloud evolution, and only develop a distinct power-law tail with index α ≃ 2 at greater column density when supercritical pockets are formed.

Abstract Copyright: © 2017 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society

Journal keyword(s): MHD - stars: formation - ISM: clouds - ISM: magnetic fields

Simbad objects: 4

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Number of rows : 4

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 NAME Mon R2 HII 06 07 47.58 -06 22 42.6           ~ 667 2
2 NAME Polaris Flare MoC 11 00 14.8 +86 10 52           ~ 168 1
3 NAME the Pipe Nebula DNe 17 30 -25.0           ~ 351 1
4 NAME Aql Region reg ~ ~           ~ 328 0

    Equat.    Gal    SGal    Ecl

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2021.04.14-13:35:22

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