3D radiative transfer simulations of Eta Carinae's inner colliding winds - I. Ionization structure of helium at apastron

TL;DR

This study uses 3D radiative transfer simulations to analyze helium ionization in Eta Carinae's colliding winds, revealing how primary star mass-loss rates influence ionization structures and observational signatures.

Contribution

It introduces a novel application of the SimpleX algorithm to post-process 3D hydrodynamic simulations, providing new insights into helium ionization and system geometry in Eta Carinae.

Findings

Lower primary mass-loss rates increase He+ volume.

Binary orientation with apastron on our side aligns better with observations.

Variations in mass-loss rate may explain historical spectral changes.

Abstract

The highly eccentric binary system Eta Carinae shows numerous time-variable emission and absorption features. These observational signatures are the result of interactions between the complex three-dimensional (3D) wind-wind collision regions and photoionization by the luminous stars. Specifically, helium presents several interesting spectral features that provide important clues on the geometry and physical properties of the system and the individual stars. We use the SimpleX algorithm to post-process 3D smoothed particle hydrodynamics simulation output of the interacting winds in Eta Car in order to obtain the fractions of ionized helium assuming three different primary star mass-loss rates. The resultant ionization maps constrain the regions where helium is singly- and doubly-ionized. We find that reducing the primary's mass-loss rate increases the volume of He+. Lowering the primary mass-loss rate produces large variations in the volume of He+ in the pre-shock primary wind on the periastron side of the system. Our results show that binary orientations in which apastron is on our side of the system are more consistent with available observations. We suggest that small variations in the primary's mass-loss rate might explain the observed increase in HeI absorption in recent decades, although numerous questions regarding this scenario remain open. We also propose that the absence of broad HeI lines in the spectra of Eta Car between its 1890's eruption and 1944 might be explained by the companion star's He0+ ionizing photons not being able to penetrate the wind-wind interaction region, due to a higher primary mass-loss rate at that time (by a factor >2, compared to the present value).