Optical Super-orbital Modulation of SMC X-1: Disk Precession and a Revised Pulsar Mass

TL;DR

This study analyzes optical and X-ray light curves of SMC X-1, revealing disk precession effects and refining the pulsar mass estimate to about 1.35 solar masses through a modified irradiation model.

Contribution

It introduces a modified ellipsoidal modulation model accounting for disk precession and irradiation effects, improving pulsar mass estimation accuracy.

Findings

Systematic optical and X-ray light curve variations synchronized with super-orbital modulation.

Model successfully reproduces observed light curves considering disk precession.

Corrected pulsar mass estimate of approximately 1.35 solar masses.

Abstract

The observational determination of the lower limit of neutron star masses is crucial for the physics of core-collapse supernovae. In this light, SMC X-1 is an important object because of its estimated pulsar mass lying near or potentially below the theoretical lower limit. SMC X-1 exhibits a double peaked optical orbital light curve due to the tidal distortion of the donor star, and analysis of this allows us to constrain the binary parameters. In this study, we analyzed optical and X-ray light curves of SMC X-1 obtained by Transiting Exoplanet Survey Satellite and Monitor of All-sky X-ray Image. We found the systematic variations in the optical orbital light curves synchronized with the X-ray super-orbital modulation, regarding the following two aspects: the minimum at inferior conjunction and the double-peak asymmetry. To explain this behavior, we developed a modified ellipsoidal modulation model in which the precessing accretion disk changes the geometry of X-ray irradiation on the donor and that of optical irradiation on the disk. As a result, this model succeeded in reproducing the observed optical and X-ray light curves. Furthermore, we discovered that intense X-ray irradiation could cause the optical emission center to shift away from the gravitational center, potentially leading to an underestimation of the radial velocity of the donor by approximately 20%. Correcting for this effect yields an updated pulsar mass estimation of about $1.35\>M_\odot$.