On the distribution of pulsars in the galactic plane

Details On the distribution of pulsars in the galactic plane On the distribution of pulsars in the galactic plane

Dec 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981a%26a...104...83d&link_type=abstract

Astronomy and Astrophysics, vol. 104, no. 1, Dec. 1981, p. 83-87.

Astronomy and Astrophysics

Astrophysics

12

Electron Density Profiles, Milky Way Galaxy, Pulsars, Spatial Distribution, Star Distribution, Astronomical Models, Correlation, Galactic Nuclei, Galactic Structure, H Ii Regions, Interstellar Gas, Stellar Evolution, Stellar Mass Ejection, Supernovae

Scientific paper

The spatial distribution of the projections of pulsars on the galactic plane within distances less than 5 kpc is determined by studying the spatial correlation between these projections and those of the H II regions of known distances. A very simple model of interstellar electron density is used to reduce the number of intervening parameters. A significant correlation appears when pulsar distances are calculated from the dispersion measurements using a mean interstellar electron density of 0.03/cu cm, considered to be uniform within the given solar neighborhood; this correlation remains when the electron density increases toward the galactic center. These correlations imply that pulsars are objects that originated from young stars, an argument which supports the type II supernova explosions theory (Guseinov and Kasumov, 1978; Tammann, 1978; Chevalier, 1980). An upper limit for their mean lifetimes is established at 10,000,000 years, which agrees with previously obtained values (Manchester, 1979; Guseinov and Kasumov, 1980).

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