Sign on

SAO/NASA ADS Astronomy Abstract Service

· Find Similar Abstracts (with default settings below)
· Electronic Refereed Journal Article (HTML)
· Full Refereed Journal Article (PDF/Postscript)
· arXiv e-print (arXiv:astro-ph/0602070)
· References in the article
· Citations to the Article (6) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (5)
· Reads History
·
· Translate This Page
Title:
A dynamical model for the dusty ring in the Coalsack
Authors:
Hennebelle, P.; Whitworth, A. P.; Goodwin, S. P.
Affiliation:
AA(École Normale Supérieure, Laboratoire de Radioastronomie Millimétrique, 24 rue Lhomond, 75231 Paris Cedex 05, France ), AB(School of Physics and Astronomy, Cardiff University, 5 The Parade, Cardiff CF24 3YB, Wales, UK ), AC(Department of Physics and Astronomy, University of Sheffield, Hicks Building, Housfield Road, Sheffield S3 7RH, UK )
Publication:
Astronomy and Astrophysics, Volume 451, Issue 1, May III 2006, pp.141-146 (A&A Homepage)
Publication Date:
05/2006
Origin:
EDP Sciences
Astronomy Keywords:
ISM: clouds, stars: formation, hydrodynamics, instabilities, shock waves
DOI:
10.1051/0004-6361:20054634
Bibliographic Code:
2006A&A...451..141H

Abstract

Lada et al. recently presented a detailed near-infrared extinction map of Globule G2 in the Coalsack molecular cloud complex, showing that this starless core has a well-defined central extinction minimum. We propose a model for G2 in which a rapid increase in external pressure is driving an approximately symmetric compression wave into the core. The rapid increase in external pressure could arise because the core has recently been assimilated by the Coalsack cloud complex, or because the Coalsack has recently been created by two large-scale converging flows. The resulting compression wave has not yet converged on the centre of the core, so there is a central rarefaction. The compression wave has increased the density in the swept-up gas by about a factor of ten, and accelerated it inwards to speeds of order 0.4 km s-1. It is shown that even a low initial level of turbulence completely destroys the coherence of the ring, as seen in projection. In the scenario of strong external compression that we are proposing this implies that the initial turbulent energy in the globule was low, ETURB/|EGRAV| ≤ 2%. Protostar formation should occur in about 40 000 years.
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)
  New!

Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints