Physical modeling of viscous disc evolution around magnetized neutron star. Aql X-1 2013 outburst decay

TL;DR

This paper develops a detailed physical model of viscous accretion disc evolution around magnetized neutron stars, explaining observed X-ray and optical light curves during outburst decay, and highlights the role of magnetic fields and disc dynamics.

Contribution

It introduces a comprehensive model incorporating magnetic interactions, disc cooling, and outflows, providing new insights into the decay phase of neutron star outbursts.

Findings

Fast flux drop explained by disc shrinking

Models with magnetic field >10^8 G fit observations better

Plateau emission can result from stalled accretion in the disc reservoir

Abstract

We present a model of a viscously evolving accretion disc around a magnetized neutron star. The model features the varying outer radius of the hot ionized part of the disc due to cooling and the varying inner radius of the disc due to interaction with the magnetosphere. It also includes hindering of accretion on the neutron star because of the centrifugal barrier and irradiation of the outer disc and companion star by X-rays from the neutron star and disc. When setting inner boundary conditions, we take into account that processes at the inner disc occur on a time scale much less than the viscous time scale of the whole disc. We consider three types of outflow from the disc inner edge: zero outflow, one based on MHD calculations, and a very efficient propeller mechanism. The light curves of an X-ray transient after the outburst peak can be calculated by a corresponding, publicly available code. We compare observed light curves of the 2013 burst of Aql X-1 in X-ray and optical bands with modeled ones. We find that the fast drop of the $0.3-10$ keV flux can be solely explained by a radial shrinking of the hot disc. At the same time, models with the neutron star magnetic field $>10^8$ G have better fits because the accretion efficiency behaviour emphasizes the 'knee' on the light curve. We also find that a plato emission can be produced by a disc-reservoir with stalled accretion.