A determination of the white-dwarf masses in wide binary radio-pulsar systems

Details A determination of the white-dwarf masses in wide binary radio-pulsar systems A determination of the white-dwarf masses in wide binary radio-pulsar systems

Jan 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987natur.325..416s&link_type=abstract

Nature (ISSN 0028-0836), vol. 325, Jan. 29, 1987, p. 416-418.

Statistics

Computation

28

Binary Stars, Pulsars, Stellar Evolution, Stellar Mass, White Dwarf Stars, Computational Astrophysics, Mass Transfer, Radio Stars, Roche Limit, Stellar Gravitation

Scientific paper

It is shown here that the fact that four of the seven known binary pulsar systems appear to fit neatly into the evolutionary scheme for bright X-ray sources described by Webbink et al. (1983) implies that a new constraint can be applied to the orbital solution of binary pulsars. This constraint is that the (sub)giant progenitor of the present white dwarf secondary should have filled its Roche lobe while spinning up the pulsar companion by mass transfer. With this extra constraint, the mass of the present white dwarf in these systems can be determined. It also permits an upper limit of about 1.2 solar mass to be set to the mass of the neutron star PSR1855 + 09.

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