Speaker
Description
Neutron stars are ultra-dense remnants of massive stellar cores, observable across the electromagnetic spectrum. Their emission reflects a complex interplay of magnetic, thermal, and structural processes operating under extreme conditions of density, temperature, and magnetic field strength that cannot be reproduced in terrestrial laboratories. Understanding isolated neutron stars therefore requires studying the physics of their interiors, where microphysical processes strongly influence both magnetic field evolution and stellar cooling. In this talk, I will introduce MATINS, a new open-access 3D code developed to model the coupled magneto-thermal evolution of isolated neutron stars. I will first discuss neutron star cooling, focusing on how observations of three faint, young neutron stars place new constraints on the nuclear equation of state. I will then turn to the physics governing magnetic field evolution, with particular emphasis on magnetars and the origin of their large-scale dipolar magnetic fields responsible for rapid spin-down. In this context, I will discuss the role of the chiral magnetic effect, arising from the chiral anomaly, which enables the mutual conversion between magnetic helicity and electron chiral asymmetry. Finally, in the last part of the talk, I will discuss finite-temperature equations of state relevant for describing hot compact objects, such as those encountered in the late stages of proto-neutron star evolution and in neutron star merger remnants.