Skip to main content

Kinetic energy decay rates of supersonic and super-alfvénic turbulence in star-forming clouds

Low, M.-M.M., Klessen, R.S., Burkert, A., Smith, M.D. (1998) Kinetic energy decay rates of supersonic and super-alfvénic turbulence in star-forming clouds. Physical Review Letters: Moving Physics Forward, 80 (13). pp. 2754-2757. ISSN 0031-9007. (doi:10.1103/PhysRevLett.80.2754) (The full text of this publication is not currently available from this repository. You may be able to access a copy if URLs are provided)

The full text of this publication is not currently available from this repository. You may be able to access a copy if URLs are provided. (Contact us about this Publication)
Official URL
http://dx.doi.org/10.1103/PhysRevLett.80.2754

Abstract

We compute 3D models of supersonic, sub-Alfvénic, and super-Alfvénic decaying turbulence, with an isothermal equation of state appropriate for star-forming interstellar clouds of molecular gas. We find that in 3D the kinetic energy decays as t-?, with 0.85 < ? < 1.2. In ID magnetized turbulence actually decays faster than unmagnetized turbulence. We compared different algorithms, and performed resolution studies reaching 2563 zones or 703 particles. External driving must produce the observed long lifetimes and supersonic motions in molecular clouds, as undriven turbulence decays too fast.

Item Type: Article
DOI/Identification number: 10.1103/PhysRevLett.80.2754
Subjects: Q Science > QB Astronomy > QB460 Astrophysics
Divisions: Faculties > Sciences > School of Physical Sciences > Centre for Astrophysics and Planetary Sciences
Depositing User: Giles Tarver
Date Deposited: 11 Aug 2015 10:23 UTC
Last Modified: 29 May 2019 15:55 UTC
Resource URI: https://kar.kent.ac.uk/id/eprint/50143 (The current URI for this page, for reference purposes)
  • Depositors only (login required):