2016MNRAS.459.2432V


C.D.S. - SIMBAD4 rel 1.7 - 2021.04.18CEST11:49:49

2016MNRAS.459.2432V - Mon. Not. R. Astron. Soc., 459, 2432-2443 (2016/July-1)

Modelling the structure of molecular clouds - I. A multiscale energy equipartition.

VELTCHEV T.V., DONKOV S. and KLESSEN R.S.

Abstract (from CDS):

We present a model for describing the general structure of molecular clouds (MCs) at early evolutionary stages in terms of their mass-size relationship. Sizes are defined through threshold levels at which equipartitions between gravitational, turbulent and thermal energy |W| ∼ f(Ekin + Eth) take place, adopting interdependent scaling relations of velocity dispersion and density and assuming a lognormal density distribution at each scale. Variations of the equipartition coefficient 1 <= f <= 4 allow for modelling of star-forming regions at scales within the size range of typical MCs (>=4 pc). Best fits are obtained for regions with low or no star formation (Pipe, Polaris) as well for such with star-forming activity but with nearly lognormal distribution of column density (Rosette). An additional numerical test of the model suggests its applicability to cloud evolutionary times prior to the formation of first stars.

Abstract Copyright: © 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society

Journal keyword(s): turbulence - methods: statistical - ISM: clouds - ISM: evolution - ISM: structure - ISM: structure

Simbad objects: 6

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Number of rows : 6

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 Perseus Cloud SFR 03 35.0 +31 13           ~ 1131 0
2 NAME Per Region reg 03 37 00.0 +31 15 00           ~ 236 0
3 NAME Ori A MoC 05 38 -07.1           ~ 2757 0
4 NAME Rosette Molecular Cloud MoC 06 34.7 +04 02           ~ 233 0
5 NAME Polaris Flare MoC 11 00 14.8 +86 10 52           ~ 168 1
6 NAME the Pipe Nebula DNe 17 30 -25.0           ~ 351 1

    Equat.    Gal    SGal    Ecl

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2021.04.18-11:49:49

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