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 (283) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (3)
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Stochastic star formation and spiral structure of galaxies
Authors:
Gerola, H.; Seiden, P. E.
Affiliation:
AA(IBM Thomas J. Watson Research Center, Yorktown Heights, N.Y.), AB(IBM Thomas J. Watson Research Center, Yorktown Heights, N.Y.)
Publication:
Astrophysical Journal, Part 1, vol. 223, July 1, 1978, p. 129-135, 137, 139. (ApJ Homepage)
Publication Date:
07/1978
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
Astronomical Models, Galactic Structure, Spiral Galaxies, Star Formation, Stochastic Processes, Astrophysics, Galactic Evolution, Shock Wave Propagation, Star Distribution
DOI:
10.1086/156243
Bibliographic Code:
1978ApJ...223..129G

Abstract

A model of self-propagating star formation (SPSF) in a two-dimensional differentially rotating disk is examined in order to determine its suitability as a model for real galactic evolution and the important parameters for ascertaining the features of known galactic structure. The model is rendered stochastic insteady of completely deterministic by introducing a finite probability for star formation, and the discrete array selected to represent a galaxy is extended to a size large enough to ensure that finite-size effects do not dominate the results. The analysis indicates that stochastic SPSF produces large-scale spiral features that are stable over long times of the order of the lifetime of a galaxy and that these features, given by the loci of star formation, rotate 'quasi-rigidly'. The spiral structure obtained using the observed rotation curves for M81 (Sb) and M101 (Sc) are shown to correspond very well with the appearance of the arms in these galaxies (e.g., pitch angle and arm density). It is found that each morphological type appears to be due simply to the rotation curve that exists in the galaxy; i.e., there is no evolution between morphological types in this model.

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