Tracing the colliding winds of $\eta$ Carinae in He I

TL;DR

This study analyzes He I line profiles from $$ Carinae to understand the geometry and dynamics of its colliding stellar winds, using a geometrical model fitted to observational data.

Contribution

It introduces a hyperboloid geometrical model of colliding winds that fits observed absorption velocities, providing insights into wind momentum balance and geometry.

Findings

Absorption lines are detected only around apastron and deviate from orbital velocities.

The geometrical model aligns with observations and simulations of $$ Carinae.

The model is highly sensitive to the wind momentum ratio and can probe wind geometry.

Abstract

$\eta$ Carinae is an extremely luminous and energetic colliding-wind binary. The combination of its orbit and orientation, with respect to our line of sight, enables direct investigation of the conditions and geometry of the colliding winds. We analyse optical He I 5876 and 7065 $\unicode{x212B}$ line profiles from the Global Jet Watch observatories covering the last 1.3 orbital periods. The sustained coverage throughout apastron reveals the distinct dynamics of the emitting versus absorbing components: the emission lines follow orbital velocities whilst one of the absorption lines is detected only around apastron ($0.08 < \phi < 0.95$) and exhibits velocities that deviate substantially from the orbital motion. To interpret these deviations, we conjecture that this He I absorption component is formed in the post-shock primary wind, and is only detected when our line of sight intersects with the shock cone formed by the collision of the two winds. We formulate a geometrical model for the colliding winds in terms of a hyperboloid in which the opening angle and location of its apex are parameterised in terms of the ratio of the wind momentum of the primary star to that of companion. We fit this geometrical model to the absorption velocities, finding results that are concordant with the panchromatic observations and simulations of $\eta$ Carinae. The model presented here is an extremely sensitive probe of the exact geometry of the wind momentum balance of binary stars, and can be extended to probe the latitudinal dependence of mass loss.