Non-steady state accretion and evolution of HER X-1 like systems

Details Non-steady state accretion and evolution of HER X-1 like systems Non-steady state accretion and evolution of HER X-1 like systems

Jan 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996mnras.278..471u&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 278, Issue 2, pp. 471-478.

Astronomy and Astrophysics

Astronomy

14

Binaries: Close, Stars: Evolution, Stars: Magnetic Fields, Stars: Neutron, Pulsars: General, Pulsars: Individual: Her X-1

Scientific paper

The magnetic evolution of pulsars in binary systems is strongly influenced by accretion. Accretion-induced heating of the neutron star interior decreases the crustal conductivity and results in a relatively rapid magnetic field decay if the field is maintained by currents in the crust. The surface field strength is determined by both the accretion rate and the duration of the accretion phase (or, in other words, the total amount of accreted mass). In the present paper, we consider the magnetic evolution of the neutron star at the beginning of the accretion phase when neither the accretion rate nor the internal temperature has reached a steady state. Our calculations show that the field can be reduced by only a small factor during the first 10^4-10^5 yr after the onset of the accretion in spite of a high accretion rate in this period, provided that the currents supporting the field structure are concentrated in the deep crustal layers. This result can account for the strong observable magnetic fields (>=10^12 G) of pulsars in Her X-1 like systems where the accretion rate is as high as 10^-8-10^-9 M_solar yr^-1. In these systems accretion probably started not long ago, but the pulsar is old enough to allow for a diffusion of the field down to the crust-core boundary.

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