Precession and Nutation in the eta Carinae binary system: Evidences from the X-ray light curve

TL;DR

This study models the X-ray light curve of eta Carinae as a binary system, incorporating precession and nutation of the primary star's rotation axis to explain observed asymmetries and oscillations.

Contribution

It introduces a novel explanation involving axis tilt, precession, and nutation to account for complex features in eta Carinae's X-ray emissions.

Findings

Reproduced main features of the X-ray light curve.

Identified axis tilt of 29 degrees as key factor.

Explained quasi-periodic oscillations with 22-day nutation period.

Abstract

It is believed that eta Carinae is actually a massive binary system, with the wind-wind interaction responsible for the strong X-ray emission. Although the overall shape of the X-ray light curve can be explained by the high eccentricity of the binary orbit, other features like the asymmetry near periastron passage and the short quasi-periodic oscillations seen at those epochs, have not yet been accounted for. In this paper we explain these features assuming that the rotation axis of eta Carinae is not perpendicular to the orbital plane of the binary system. As a consequence, the companion star will face eta Carinae on the orbital plane at different latitudes for different orbital phases and, since both the mass loss rate and the wind velocity are latitude dependent, they would produce the observed asymmetries in the X-ray flux. We were able to reproduce the main features of the X-ray light curve assuming that the rotation axis of eta Carinae forms an angle of 29 degrees with the axis of the binary orbit. We also explained the short quasi-periodic oscillations by assuming nutation of the rotation axis, with amplitude of about 5 degrees and period of about 22 days. The nutation parameters, as well as the precession of the apsis, with a period of about 274 years, are consistent with what is expected from the torques induced by the companion star.