Astronomy and Astrophysics – Astrophysics
Scientific paper
Aug 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985a%26a...149..283s&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 149, no. 2, Aug. 1985, p. 283-290.
Astronomy and Astrophysics
Astrophysics
5
Binary Stars, Gravitational Collapse, Stellar Evolution, Stellar Orbits, Constraints, Energy Dissipation, Gravitational Waves, Pulsars, Stellar Rotation
Scientific paper
In the present examination of the clean relativistic binary star orbital period change induced by evolutionary self-energy losses of collapsed members, it is noted that the orbital energy change is dominated by the emission of gravitational radiation rather than self-energy losses due to rotational slowing and possible contraction of the members. In the case of the binary pulsar PSR 1913 + 16, the possibly nonvanishing difference between observed and predicted values of the orbital period shortening cannot be due to post-Newtonian orbital effects; it is also too large to be attributable to the members' combined slowing. Using the companion's estimated rotational and contractional absolute luminosities, extreme bounds are proposed for the rotation period and its rate of change, surface magnetic field induction, surface absolute temperature, contraction rate, and intensity-peak frequency. The conformity of the contraction property with the phenomena of the pulsars' glitches is also examined.
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