Signs of magnetic accretion in young Be/X-ray pulsar SXP 1062

TL;DR

This paper investigates the rapid spin-down of the young Be/X-ray pulsar SXP 1062, proposing magnetic accretion from a magnetized wind as the explanation, and estimates the neutron star's magnetic field and age.

Contribution

It introduces magnetic accretion as a viable scenario to explain the pulsar's spin-down, addressing limitations of conventional models.

Findings

Spin-down rate explained by magnetic accretion with B_* ~ 4 x 10^{13} G

Estimated pulsar age between 20,000 and 40,000 years

Conventional accretion scenarios face difficulties explaining observed spin behavior

Abstract

The spin behaviour of the neutron star in the newly discovered young Be/X-ray long-period pulsar SXP 1062 is discussed. The star is observed to rotate with the period of 1062s, and spin-down at the rate ~ - 2.6 \times 10^{-12} Hz s^{-1}. I show that all of the conventional accretion scenarios encounter major difficulties explaining the rapid spin-down of the pulsar. These difficulties can be, however, avoided within the magnetic accretion scenario in which the neutron star is assumed to accrete from a magnetized wind. The spin-down rate of the pulsar can be explained within this scenario provided the surface magnetic field of the neutron star is B_* ~ 4 \times 10^{13} G. I show that the age of the pulsar in this case lies in the rage (2-4) \times 10^4 yr, which is consistent with observations. The spin evolution of the pulsar is briefly discussed.