Modeling the RXTE light curve of $\eta$ Carinae from a 3-D SPH simulation of its binary wind collision

TL;DR

This study uses 3-D SPH simulations to model the binary wind collision in $eta$ Carinae, successfully fitting the RXTE X-ray light curve and constraining the system's orbital geometry and orientation.

Contribution

It introduces a comprehensive 3-D dynamical model of $eta$ Carinae's wind collision, linking simulation results with observed X-ray variability to determine orbital parameters.

Findings

The RXTE light curve fits well with an inclination of 45°.

The orbital position angle is constrained to about 27°.

The model confirms the wind collision geometry explains observed X-ray variations.

Abstract

The very massive star system $\eta$ Carinae exhibits regular 5.54-year (2024-day) period disruptive events in wavebands ranging from the radio to X-ray. There is a growing consensus that these events likely stem from periastron passage of an (as yet) unseen companion in a highly eccentric ($\epsilon \sim 0.9$) orbit. This paper presents three-dimensional (3-D) Smoothed Particle Hydrodynamics (SPH) simulations of the orbital variation of the binary wind-wind collision, and applies these to modeling the X-ray light curve observed by the Rossi X-ray Timing Explorer (RXTE). By providing a global 3-D model of the phase variation of the density of the interacting winds, the simulations allow computation of the associated variation in X-ray absorption, presumed here to originate from near the apex of the wind-wind interaction cone. We find that the observed RXTE light curve can be readily fit if the observer's line of sight is within this cone along the general direction of apastron. Specifically, the data are well fit by an assumed inclination $i = 45^{\circ}$ for the orbit's polar axis, which is thus consistent with orbital angular momentum being along the inferred polar axis of the Homunculus nebula. The fits also constrain the position angle $\phi$ that an orbital-plane projection makes with the apastron side of the semi-major axis, strongly excluding positions $\phi < 9^{\circ}$ along or to the retrograde side of the axis, with the best fit position given by $\phi = 27^{\circ}$. Overall the results demonstrate the utility of a fully 3-D dynamical model for constraining the geometric and physical properties of this complex colliding-wind binary system.