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A. Spitkovsky (KIPAC, Stanford University), J. Arons (UC Berkeley)
Confinement of the magnetosphere of pulsar J0737-3039B by the powerful wind from millisecond pulsar J0737-3039A provides a unique probe of the physics of pulsar winds and magnetospheres. We present simulations of the interaction between the magnetized relativistic wind from pulsar A with the magnetosphere of pulsar B, which is modeled as an inclined rotating magnetic dipole. Using a particle-in-cell code we obtain the 3D time-dependent shape of the B's magnetosphere including the stand-off collisionless shock and the magnetosheath, which is reminiscent of a terrestrial magnetosphere. We find that for large inclination angles between magnetic and rotational axes of B the shape of the magnetosheath is skewed by B's rotation, and that the shocked wind plasma streams into B's magnetosphere preferentially on the side that is moving in downwind direction. These "cusps" introduce time-averaged asymmetry in the shape of the magnetosheath which is potentially responsible for asymmetry in the morphology of A's eclipse by B.
We also consider the properties of the B pulsar related to the confinement of its magnetosphere by the wind. Reconnection with magnetic field of the wind at favorable rotation phases of B causes torque on the magnetosphere which is comparable to the value of standard electromagnetic spindown for B. We simulate these reconnection events and compare simulations with analytical estimates of the propellor torque. We also show how variation of polar cap size with rotation of B together with changes in mutual orientation of the line of sight with magnetosheath can be used to explain the modulation of the observed emission of B with orbital phase.
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Bulletin of the American Astronomical Society, 36 #3
© 2004. The American Astronomical Soceity.