Magnetic Inhibition of Accretion and Observability of Isolated Old Neutron Stars

Abstract

Isolated old neutron stars moving through the interstellar medium capture matter gravitationally. If the star is unmagnetized, the captured matter accretes to the surface of the star. However, the stars are expected to be magnetized. Moreover, some of the stars may be in the ‘‘ propeller ’’ stage of evolution. Both the magnetic field and the rotation act to decrease the accretion rate to the surface of the star. Here we consider stars that are past the propeller stage, so that rotation is unimportant. The influence of the magnetic field on the accretion rate to the star’s surface is investigated using axisymmetric, resistive magnetohydrodynamic (MHD) simulations. Matter is taken to inflow at the Bondi rate for a nonmagnetized star, and we verify that stationary Bondi accretion flows occur in the absence of a magnetic field. For a magnetized star we find that an outward-propagating shock wave forms and that a new stationary, subsonic accretion flow is set up inside this shock, as first pointed out by Toropin et al. in 1999. Accretion to the surface of the star _ M occurs along two columns aligned with the magnetic axis of the star. Only a fraction of the Bondi flux _ MB accretes to the surface of the star. The empirical dependences we find are _ M= _