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We present magnetohydrodynamic numerical simulations of the latepost-supernova hypercritical accretion to understand its effect on the magneticfield of the new-born neutron star. We consider as an example the case of amagnetic field loop protruding from the star's surface. The accreting matter isassumed to be non magnetized and, due to the high accretion rate, matterpressure dominates over magnetic pressure. We find that an accretion envelopedevelops very rapidly and once it becomes convectively stable the magneticfield is easily buried and pushed into the newly forming neutron star crust.However, for low enough accretion rates the accretion envelope remainsconvective for an extended period of time and only partial submergence of themagnetic field occurs due to a residual field that is maintained at theinterface between the forming crust and the convective envelope. In this lattercase, the outcome should be a weakly magnetized neutron star with a likelycomplicated field geometry. In our simulations we find the transition fromtotal to partial submergence to occur around dotM ~ 10 M_sun/yr. Back-diffusionof the submerged magnetic field toward the surface, and the resulting growth ofthe dipolar component, may result in a delayed switch-on of a pulsar ontime-scales of centuries to millenia.

Hypercritical Accretion onto a Newborn Neutron Star and Magnetic Field Submergence