Characteristics of old neutron stars in dense interstellar clouds

Details Characteristics of old neutron stars in dense interstellar clouds Characteristics of old neutron stars in dense interstellar clouds

Feb 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...313..218b&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 313, Feb. 1, 1987, p. 218-225.

Astronomy and Astrophysics

Astrophysics

10

Gas Density, Interstellar Gas, Neutron Stars, Spectral Signatures, Stellar Evolution, X Ray Sources, Energy Dissipation, Gamma Ray Spectra, Molecular Clouds, Stellar Mass Accretion, Stellar Models

Scientific paper

The forms observable radiation will assume as old neutron stars pass through interstellar clouds and accrete material are examined theoretically. The radiation, mainly X-rays and gamma rays, will be partially absorbed by the surrounding dust and gas, which in turn produces far-IR radiation from warm dust and line radiation from the gas. Adiabatic compression of the accretion flow and the accretion shock are expected to produce cosmic rays, while gamma rays will be emitted by interaction of the energetic particles with the cloud material. The calculations indicate that the stars will then be identified as X-ray sources, some of which may be unidentified sources in the COS-B database.

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