Statistics – Computation
Scientific paper
Sep 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...378...93l&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 378, Sept. 1, 1991, p. 93-105. Research supported by NSF, University of Tex
Statistics
Computation
28
Computational Astrophysics, Galactic Structure, H Ii Regions, Milky Way Galaxy, Statistical Correlation, Supernova Remnants, Monte Carlo Method, Star Distribution
Scientific paper
The distribution of observed giant H II regions and supernova remnants (SNRs) in Galactic longitude is analyzed with Monte Carlo models to determine the possible correlation with spiral arms or disk populations. The novel feature of the current analysis is that it depends mainly on the angular distribution of the H II regions and SNRs and hence is independent of distance. The SNRs seem to require a long-disk-scale length. The possible correlations of the SNR distribution with the old stellar disk and the average radial distribution of the H I, H2, and total gas density in the Galaxy is discussed. The models presented incorporate selection effects in a parameterized way and suggest that about 1000 SNRs exist in the Galaxy, with about 850 remaining to be discovered. There is no substantial evidence that SNRs are especially concentrated in spiral arms as they would be if they were selectively born in spiral arms or if the high gas density in the arms were the dominant selection effect for the production of long-lived remnants. On the basis of the current evidence, the hypothesis that the shell-type remnants that dominate the SNRs sample arise from old disk SN Ia events cannot be strongly rejected. The H II region distribution is not especially well fitted with any of the models but suggests a radial scale length in the solar neighborhood of about 3.5 kps, substantially less than the SNR distribution.
Bash Frank N.
Jefferys William H.
Li Zongwei
Wheeler Justin C.
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