Speaker
Description
Accretion onto the first-born neutron star during a super-Eddington episode has been proposed as one of the formation channels of the most massive neutron stars in the gravitational-wave catalogue, notably the components of GW190425. In this work, we examine the transfer of material from the outer disc to the stellar surface during the super-Eddington phase. We take into account the disc truncation at the magnetospheric radius and radiatively driven winds. The magnetic moment, spin and baryonic mass of the neutron star are evolved as a coupled system, incorporating accretion-induced field burial and Ohmic re-emergence, with baryonic mass converted to gravitational mass along the track. The retained fraction that emerges depends on the disc wind index, the magnetic moment, the mass-transfer rate and the spin period, and we map this dependence across the plausible parameter space. We test our results against the mass–spin distribution of Galactic recycled pulsars and the gravitational-wave mass measurements.