Sign on

SAO/NASA ADS Astronomy Abstract Service


· Find Similar Abstracts (with default settings below)
· Full Refereed Journal Article (PDF/Postscript)
· Full Refereed Scanned Article (GIF)
· References in the article
· Citations to the Article (692) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (2)
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Magnetohydrodynamic shock waves in molecular clouds
Authors:
Draine, B. T.; Roberge, W. G.; Dalgarno, A.
Affiliation:
AA(Institute for Advanced Study, Princeton, NJ), AB(Institute for Advanced Study, Princeton, NJ; Harvard-Smithsonian Center for Astrophysics, Cambridge, MA), AC(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA)
Publication:
Astrophysical Journal, Part 1, vol. 264, Jan. 15, 1983, p. 485-507. (ApJ Homepage)
Publication Date:
01/1983
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
Interstellar Gas, Magnetohydrodynamic Waves, Molecular Clouds, Shock Waves, Hydrogen, Infrared Spectra, Interstellar Magnetic Fields, Molecular Excitation, Molecular Interactions, Momentum Transfer, Plane Waves, Wave Propagation
DOI:
10.1086/160617
Bibliographic Code:
1983ApJ...264..485D

Abstract

Calculations for the structure of shock waves in molecular clouds are presented which include the effects of ion-neutral streaming driven by the magnetic field. Results show that shock waves in molecular clouds will usually be C-type shock waves, mediated entirely by the dissipation accompanying ion-neutral streaming, and in which all of the hydrodynamic variables are continuous. The magnetohydrodynamic shock waves propagating at speeds in the range of 5-50 km/s in molecular clouds with preshock densities n(H) = 100, 10000, and 1000000/cu cm are studied in detail. The effects of chemical changes in the composition of oxygen-bearing molecules are determined, and the contributions to the cooling of the shocked gas by emission from H2, CO, OH, and H2O are evaluated. The intensities of the rotation-vibration lines of H2 and of the fine-structure lines of O I and C I are predicted. It is shown that magnetic fields may lead to a substantial increae in the limiting shock velocity above which dissociation of H2 takes place, such that for a cloud of intensity n(H) = 1000000/cu cm, the limiting shock speed is approximately 45 km/s.

Printing Options

Print whole paper
Print Page(s) through

Return 600 dpi PDF to Acrobat/Browser. Different resolutions (200 or 600 dpi), formats (Postscript, PDF, etc), page sizes (US Letter, European A4, etc), and compression (gzip,compress,none) can be set through the Printing Preferences



More Article Retrieval Options

HELP for Article Retrieval


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