Magnetic moments of neutron stars with different equations of state

Details Magnetic moments of neutron stars with different equations of state Magnetic moments of neutron stars with different equations of state

Mar 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986afz....24..279s&link_type=abstract

(Astrofizika, vol. 24, Mar.-Apr. 1986, p. 279-286) Astrophysics (ISSN 0571-7132), vol. 24, no. 2, Sept. 1986, p. 163-166. Transl

Astronomy and Astrophysics

Astrophysics

1

Magnetic Moments, Neutron Stars, Stellar Magnetic Fields, Density Distribution, Equations Of State, Pulsar Magnetospheres, Superfluidity

Scientific paper

The magnetic field of a neutron star in the npe stage is investigated theoretically, extending the analysis of Sedrakian et al. (1984) to stable superdense configurations described by the equations of state of Saakian (1972), Pandharipande (1971), and Bayme et al. (1971). The dragging of superfluid protons by rotating superfluid neutrons is found to produce (1-10) x 10 to the 29th G cu cm magnetic moments parallel to the rotation axis of the stars. The implications of this finding for the theory of pulsar magnetospheres and emission are indicated.

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