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)
· References in the article
· Citations to the Article (2) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (5)
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Hydrodynamic simulations of rotating molecular jets
Authors:
Smith, Michael D.; Rosen, Alexander
Affiliation:
AA(Armagh Observatory, College Hill, Armagh BT61 9DG; Centre for Astrophysics & Planetary Science, The University of Kent, Canterbury, Kent CT2 7NH), AB(Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, D-53121 Bonn, Germany)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 378, Issue 2, pp. 691-700. (MNRAS Homepage)
Publication Date:
06/2007
Origin:
MNRAS
MNRAS Keywords:
hydrodynamics , shock waves , ISM: clouds , ISM: jets and outflows , ISM: molecules
Abstract Copyright:
(c) 2007 The Authors. Journal compilation © 2007 RAS
DOI:
10.1111/j.1365-2966.2007.11816.x
Bibliographic Code:
2007MNRAS.378..691S

Abstract

Molecular outflows and the jets which may drive them can be expected to display signatures associated with rotation if they are the channels through which angular momentum is extracted from material accreting on to protostars. Here, we determine some basic signatures of rapidly rotating flows through three-dimensional numerical simulations of hydrodynamic jets with molecular cooling and chemistry. We find that these rotating jets generate a broad advancing interface which is unstable and develops into a large swarm of small bow features. In comparison to precessing jets, there is no stagnation point along the axis. The greater the rotation rate, the greater the instability. On the other hand, velocity signatures are only significant close to the jet inlet since jet expansion rapidly reduces the rotation speed. We present predictions for atomic, H2 and CO submillimetre images and spectroscopy including velocity channel maps and position-velocity diagrams. We also include simulated images corresponding to Spitzer IRAC band images and CO emission, relevant for APEX and eventual ALMA observations. We conclude that protostellar jets often show signs of slow precession but only a few sources display properties which could indicate jet rotation.
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)
   

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
    


SAO/NASA ADS Homepage | ADS Sitemap | Query Form | Basic Search | Preferences | HELP | FAQ