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 (94) (Citation History)
· Refereed Citations to the Article
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Molecular evolution of contracting clouds - Basic methods and initial results
Authors:
Gerola, H.; Glassgold, A. E.
Affiliation:
AA(IBM Thomas J. Watson Research Center, Yorktown Heights, N.Y.), AB(New York University, New York, N.Y.)
Publication:
Astrophysical Journal Supplement Series, vol. 37, May 1978, p. 1-25. (ApJS Homepage)
Publication Date:
05/1978
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
Chemical Evolution, Hydrogen Clouds, Interstellar Chemistry, Interstellar Gas, Molecular Gases, Nebulae, Clouds, Gas Density, Gas Temperature, Radiative Heat Transfer, Thermodynamics
DOI:
10.1086/190515
Bibliographic Code:
1978ApJS...37....1G

Abstract

The relationship between the dynamics of the interstellar gas and the thermal and chemical effects associated with interstellar molecules and dust is investigated. The evolution of a rather massive isolated initially diffuse cloud under self-gravity is studied, using the equations of hydrodynamics; only radial motions are considered, and the heat, chemical, and radiative-transfer equations are solved simultaneously with the hydrodynamic equations. The relevant chemistry is described along with the thermal model, the radiative-transfer process, and the numerical methods employed. Results for a contracting cloud are discussed in terms of the problem of initial conditions, the dynamical evolution of the cloud, its chemical and thermal evolution, time scales, and column densities. It is shown that the chemical evolution of a massive contracting diffuse cloud is sensitive to such physical properties as temperature and ion abundances, that warm and cool versions of a typical cloud evolve differently, and that the physical origin of this effect is the level of heating due to H2 formation on interstellar dust grains.

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)

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