Accretion in the spin-down regime

Details Accretion in the spin-down regime Accretion in the spin-down regime

Sep 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aipc.1379..156e&link_type=abstract

ASTROPHYSICS OF NEUTRON STARS 2010: A Conference in Honor of M. Ali Alpar. AIP Conference Proceedings, Volume 1379, pp. 156-159

Astronomy and Astrophysics

Astrophysics

X-Ray Sources (Astronomical), Flare Stars, Brightness, Plasma, X-Ray Sources, X-Ray Bursts, Flare Stars, Luminosities, Magnitudes, Effective Temperatures, Colors, And Spectral Classification, Magnetohydrodynamics And Plasmas

Scientific paper

Accretion driven millisecond X-ray pulsars can accrete over a wide range of mass flow rates. The pulsations persist even at small accretion rates at which these objects would be expected to be in the propeller stage. We argue that the inner regions of disks around millisecond X-ray pulsars are sufficiently thick that a fraction of the inflowing matter can accrete even in the spin-down regime from regions of the disk away from the disk plane. This allows these systems to be bright throughout a wide range of mass flow rates. We model the lightcurve of SAX J1808.4-3658 during an outburst and show that the rapid decay stage can be modeled with fractional accretion in the spin-down regime.

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