Computer Science
Scientific paper
May 1979
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979natur.279..401m&link_type=abstract
Nature, Volume 279, Issue 5712, pp. 401-402 (1979).
Computer Science
8
Scientific paper
THE presence of rotating neutron stars in binary systems is revealed by the existence of X-ray pulsators which are generally associated with massive companions. The evolutionary history of these systems is now relatively clear (see ref. 1 and refs therein). The X-ray phase, which corresponds to accretion on the neutron star of a strong stellar wind Ṁ ~ 10-6 Msolar yr-1, is preceded by a much longer quiet state, where the primary is unevolved, possibly with a weak wind, Ṁ ~ 10-9 Msolar yr-1 and the rotational energy loss of the neutron star inhibits accretion. However, with the only exception of PSR1913 + 16, radio pulsars are not found in binary systems. Here, motivated by the recent discovery of γ-ray emission from slow pulsars2,3, we suggest γ-ray observations as a way of detecting binaries in the quiet state and compare the expected number with the COS B results. We refer to the review of van den Heuvel1 where, as a representative case, a system of initial mass 20 + 8 Msolar and orbital period 4.7 d is considered. After the first stage of mass exchange and the supernova explosion, one has a neutron star with an unevolved companion of 22.7 Msolar. The period is now P = 12.6 d. The primary remains on the main sequence (quiet stage) for tms = 3.6 × 106yr. The X-ray phase occurs after the star has left the main sequence, but before it fills its Roche lobe, as an excessive mass transfer absorbs the X-ray emission. Its duration is tx ~ 104yr.
Maraschi Laura
Treves Aldo
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