Is there a highly magnetized neutron star in GX 301-2?

TL;DR

This study analyzes the long-period X-ray pulsar GX 301-2, revealing a rapid orbital decay and proposing a strong magnetic field explanation for its long pulse period, which may involve a tall accretion column.

Contribution

It introduces a model suggesting a magnetic field of ~10^{14} G for GX 301-2, reconciling cyclotron line data with the observed long pulse period.

Findings

Orbital period decays at a rate of ~-3.25 x 10^{-5} days per year.

A magnetic field of ~10^{14} G explains the long pulse period.

A tall accretion column can reconcile cyclotron line measurements.

Abstract

We present the results of an in-depth study of the long-period X-ray pulsar GX 301-2. Using archival data of INTEGRAL, RXTE ASM, and CGRO BATSE, we study the spectral and timing properties of the source. Comparison of our timing results with previously published work reveals a secular decay of the orbital period at a rate of \simeq -3.25 \times 10^{-5} d yr^{-1}, which is an order of magnitude faster than for other known systems. We argue that this is probably result either of the apsidal motion or of gravitational coupling of the matter lost by the optical companion with the neutron star, although current observations do not allow us to distinguish between those possibilities. We also propose a model to explain the observed long pulse period. We find that a very strong magnetic field B \sim 10^{14} G can explain the observed pulse period in the framework of existing models for torques affecting the neutron star. We show that the apparent contradiction with the magnetic field strength B_{CRSF} \sim 4 \times 10^{12} G derived from the observed cyclotron line position may be resolved if the line formation region resides in a tall accretion column of height \sim 2.5 - 3 R_{NS}. The color temperature measured from the spectrum suggests that such a column may indeed be present, and our estimates show that its height is sufficient to explain the observed cyclotron line position.