Period derivative and orbital eccentricity of binary pulsar 1953 + 29

Details Period derivative and orbital eccentricity of binary pulsar 1953 + 29 Period derivative and orbital eccentricity of binary pulsar 1953 + 29

Jan 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986natur.319..383r&link_type=abstract

Nature (ISSN 0028-0836), vol. 319, Jan. 30, 1986, p. 383, 384.

Astronomy and Astrophysics

Astronomy

25

Binary Stars, Eccentricity, Pulsars, Stellar Orbits, Stellar Rotation, Gamma Ray Astronomy, Stellar Evolution, Stellar Mass Accretion

Scientific paper

PSR 1953+29, the second fastest of more than 400 known pulsars, has a period of 6.133 ms and is a member of a binary system with an orbital period of 117.35 days. The authors have determined two important parameters of the system, the pulsar period derivative Pand the orbital eccentricity e. They find a small but non-zero eccentricity, e = (330.3±0.4)×10-6, and a spindown rate of P= (1±6)×10-20s s-1, smaller than that measured for any other pulsar. These values are consistent with an evolutionary history involving spin-up during a mass accretion phase.

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