An upper limit to the rate of formation of neutron stars in the Galaxy. II

Details An upper limit to the rate of formation of neutron stars in the Galaxy. II An upper limit to the rate of formation of neutron stars in the Galaxy. II

Aug 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...240..242h&link_type=abstract

Astrophysical Journal, Part 1, vol. 240, Aug. 15, 1980, p. 242-245.

Astronomy and Astrophysics

Astrophysics

8

Milky Way Galaxy, Neutron Stars, Stellar Evolution, B Stars, Energy Dissipation, Luminous Intensity, O Stars, Star Distribution

Scientific paper

The method for determining the rate of formation of neutron stars in the Galaxy is examined in relation to the substantial difference which exists between the value of about one every 27 years reported by Hills (1978) and that of one every 4 years reported by Endal (1979). The large difference is due to Endal's assumption that the stellar population in the galactic plane near the Sun is representative of the Galaxy as a whole, whereas Hills considers the stars in an infinitely long cylinder perpendicular to the galactic plane. Endal's rate of neutron-star formation and value of photon energy emitted by the average neutron-star progenitor, OB star, require that the integrated photon luminosity of the neutron-star progenitors in the Galaxy be 3.2 x 10 to the 10th solar luminosities' which is approximately 50% larger than the total photon luminosity of all stars in the Galaxy. Using different observational data, the maximum possible rate of neutron-star formation in the Galaxy obtained is one every 21 years, with a probable rate being roughly one every 48 years.

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