The slow X-ray pulsar SXP 1062 and associated supernova remnant in the Wing of the Small Magellanic Cloud

TL;DR

This paper studies the young neutron star SXP 1062 in the Small Magellanic Cloud, examining its unique properties to understand neutron star evolution and accretion physics.

Contribution

It provides new observational data to test theoretical models of neutron star evolution and accretion in high-mass X-ray binaries.

Findings

SXP 1062 is a young neutron star with a measured spin period and derivative.

The source's properties challenge existing models of neutron star spin evolution.

New data will test and refine theories of accretion and neutron star development.

Abstract

SXP 1062 is an exceptional case of a young neutron star in a wind-fed high-mass X-ray binary associated with a supernova remnant. A unique combination of measured spin period, its derivative, luminosity and young age makes this source a key probe for the physics of accretion and neutron star evolution. Theoretical models proposed to explain the properties of SXP 1062 shall be tested with new data.