Astronomy and Astrophysics – Astrophysics
Scientific paper
Aug 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991aipc..232..401b&link_type=abstract
IN: Gamma-ray line astrophysics; Proceedings of the International Symposium, Paris, France, Dec. 10-13, 1990 (A92-43619 18-90).
Astronomy and Astrophysics
Astrophysics
Equations Of State, Gamma Ray Telescopes, Neutron Stars, Red Shift, Stellar Mass Accretion, Carbon 12, Helium, Oxygen Isotopes, Radioactive Decay
Scientific paper
The current generation of gamma-ray telescopes (SIGMA, GRO) provides a new opportunity for observing red-shifted gamma-ray lines from the atmospheres of accreting neutron stars. A successful observation would provide important information about how the accretion stream settles onto the neutron star and might allow limits to be placed on the nuclear equation of state. Thus, a theoretical reanalysis of different gamma-ray emission mechanisms was undertaken. This paper describes the results on the 4.438 MeV gamma-ray line emission from C-12 and O-16 and outlines the ongoing calculation of the 2.2 MeV D-recombination line flux expected from the spallation of incident helium. It is shown that a neutron star accreting material of solar abundances will produce a 4.438 MeV gamma-ray line flux that is below the current observational limits.
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