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Non-Stationary Accretion in Her X–1–like Systems

Published online by Cambridge University Press:  12 April 2016

U. Geppert  and
V. Urpin
U. Geppert
Affiliation:
MPI für Extraterrestrische Physik, Aussenstelle, Berlin
V. Urpin
Affiliation:
MPI für Extraterrestrische Physik, Aussenstelle, Berlin

Extract

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Accretion heats the neutron star crust thereby decreasing the electric conductivity in the solid region. This leads to a rapid field decay when the currents supporting the field are concentrated in the solid crust (Geppert & Urpin 1994, Urpin & Geppert 1995). Depending on the duration of the accretion phase and on the total mass accreted the field can be decreased by 3 − 4 orders of magnitude after 106 − 107 years. This mechanism explains the low magnetic fields of many pulsars entering binary systems.

However, there exist both low–mass (e.g. Her X–1, 4U 1626–67) and high–mass (e.g. Cen X–3, SMC X–1) systems, where the neutron star deserves strong accretion and the magnetic field is still large.

Type
Part 7 Binary Systems
Information
International Astronomical Union Colloquium , Volume 160: Pulsars: Problems and Progress , 1996 , pp. 537 - 538
Copyright
Copyright © Astronomical Society of the Pacific 1996

References

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