Neutron star cores: normal matter and superconductivity

Andrei Igoshev (Newcastle University)

Wednesday 18th March 15:00-16:00
Maths 311B

Abstract

Neutron stars have the strongest magnetic fields in the Universe reaching 1e15 G. Magnetic field evolution in neutron star cores is not fully explored. Researchers still do not agree on whether neutron star cores are magnetised or whether the magnetic field is expelled very early from the cores.  According to earlier works, the core is expected to turn into a type II superconductor relatively early after the neutron star formation. The cores of magnetars with the strongest magnetic fields, are expected to stay normal for much longer. In this work, I explain our magnetohydrodynamic approach to modelling normal and superconducting neutron star cores. We develop a multi-fluid code based on Dedalus to model the long-term evolution of neutron star cores. In the normal case and in two spatial dimensions, the poloidal magnetic field evolves towards the Grad-Shafranov equilibrium. In three spatial dimensions, the field becomes unstable and form a new magnetic field configuration after a period of magnetic turbulence.  I present the key stages of the evolution. At the end, I present our preliminary results for superconducting cores.

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