Abstract
In this work I present numerical magnetohydrodynamic (MHD) simulations of the early dynamics around newly born neutrons stars using the AMR Flash method. When the core-collapse supernovae occurs a reverse shock is formed allowing strong accretion onto the neutron star surface (hypercritical phase). In such regime large amounts of matter are deposited on the neutron star surface, submerging the magnetic field in the new crust. When the hypercritical regime is over, the magnetic field can suffer a reemergence episode due to magnetic diffusion processes, allowing the delayed switch-on of pulsars.
Highlights
It is widely accepted that core-collapse supernovae are ideal laboratories for fundamental astrophysics because they exhibit extreme conditions of density and temperature not found in terrestrial environments
The two lateral sides are treated as periodic boundaries, while at the bottom the field is frozen from the initial condition, i.e., the two feet of the loop are anchored into the neutron star and no field can be pushed into the star by the accretion
I am interested in following the evolution of the magnetic field, which is anchored onto the proto-neutron star surface, when the hypercritical accretion phase take place
Summary
It is widely accepted that core-collapse supernovae are ideal laboratories for fundamental astrophysics because they exhibit extreme conditions of density and temperature not found in terrestrial environments. This reverse shock allows to deposit large amounts of matter onto the protoneutron surface forming a new crust. The analytical models that describe such hypercritical accretion onto neutron star surfaces use several assumptions: stationary flows, spherical symmetry of the flow, ideal gas as equation of state, only pair annihilation processes in the neutrino cooling process, and negligible magnetic field of the compact remnant.
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