Astronomy and Astrophysics – Astronomy
Scientific paper
Aug 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006iaujd...2e..42m&link_type=abstract
On the Present and Future of Pulsar Astronomy, 26th meeting of the IAU, Joint Discussion 2, 16-17 August, 2006, Prague, Czech Re
Astronomy and Astrophysics
Astronomy
Scientific paper
The present study is mainly addressed to the coupled spin, mass, magnetic field, orbital separation, and orbital period evolution of a neutron star entering a close binary system with a low mass main sequence companion, which loses mass in form of homogenous stellar wind. We apply flux expulsion of the magnetic field from the superfluid superconductive core of a neutron star , based on different equation of states, and its subsequent decay in the crust , which also depends on conductivity of the crust, and hence on the temperature, T, and the neutron star age. The initial core and surface magnetic field are of the same order of magnitude. To derive the rate of expulsion of the magnetic flux out of the core we consider various forces which act on the fluxoids in the interior of a neutron star, including a force due to their pinning interaction with the moving neutron vortices, buoyancy force, curvature force, and viscous drag force due to magnetic scattering of electrons. Various effects accompanying mass exchange in binaries can influence the evolution of spin and magnetic field of the neutron star. The orbital separation of the binary clearly affects the estimated value of , and it itself evolves due to mass exchange between the components, mass loss from the system, and two other sinks of the orbital angular momentum namely magnetic braking and gravitational waves. The neutron star passes through four evolutionary phases ( isolated pulsar- propeller- accretion from the wind of a companion- accretion resulting from Roche-lobe overflow). Models for a range of parameters, and initial orbital period, magnetic field and spin period are constructed. The impurity parameter, Q, is assumed to be constant during the whole evolution of the star and range from 1 to 0.001. Final magnetic field, spin and orbital period are presented in this paper. The surface magnetic field weakens by a factor of .The suggested mechanism can explain the lower magnetic field and faster spins of millisecond pulsars that have been recycled by accretion in close binaries.
Abdolrahimi Shohreh
Javadi Khasraghi Atefeh
Mirtorabi M.
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