On the slow-down of the millisecond pulsar PSR 1937 + 214

Details On the slow-down of the millisecond pulsar PSR 1937 + 214 On the slow-down of the millisecond pulsar PSR 1937 + 214

Jan 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984ap%26ss..98..203s&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 98, no. 1, Jan. 1984, p. 203-205.

Astronomy and Astrophysics

Astrophysics

2

Astrophysics, Pulsars, Stellar Magnetic Fields, Accretion Disks, Electromagnetic Radiation, Energy Dissipation, Stellar Models, Stellar Rotation

Scientific paper

There are indications that less than 10-3 of the spin-down energy of the millisecond pulsar PSR 1937+214 emerges as electromagnetic radiation. The implications of this result are discussed. The surface magnetic field would then be ≡107G, making the pulsar optically undetectable, and casting aspersions on the accretion disc spin-up neutron star models for the pulsar. The pulsar should have an equatorial ellipticity ɛ ≡ 10-9, which can be accounted for if the equatorial magnetic field departs from axisymmetry by one part in 103.

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