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Title:
Massive star formation in NGC 6946
Authors:
Degioia-Eastwood, K.; Grasdalen, G. L.; Strom, S. E.; Strom, K. M.
Affiliation:
AA(Wyoming, University, Laramie, WY), AB(Wyoming, University, Laramie, WY), AC(Kitt Peak National Observatory, Tucson, AZ), AD(Kitt Peak National Observatory, Tucson, AZ)
Publication:
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 278, March 15, 1984, p. 564-574. NSF-supported research. (ApJ Homepage)
Publication Date:
03/1984
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
DENSITY WAVE MODEL, SPIRAL GALAXIES, STAR FORMATION, STELLAR MASS, GALACTIC EVOLUTION, GALACTIC NUCLEI, GAS DENSITY, H ALPHA LINE, INTERSTELLAR MATTER, RADII, RATES (PER TIME), STAR FORMATION RATE
DOI:
10.1086/161823
Bibliographic Code:
1984ApJ...278..564D

Abstract

H-alpha measurements of the late-type spiral galaxy NGC 6946 are presented. Assuming an initial mass function, the H-alpha data are used to calculate the total star formation rate and efficiency of massive star formation as a function of galactocentric radius. An attempt is made to determine the factors influencing these quantities by comparing them to the surface densities of H I and H 2 and the degree of compression suffered by the gas in spiral density wave theory. The rate of star formation is very closely correlated with the first power of the surface density of H2, and somewhat less correlated with the degree of compression of the gas predicted by density wave theory. In contrast, the efficiency of massive star formation is roughly constant across the face of the galaxy.

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