Accretion onto the Companion of Eta Carinae During the Spectroscopic Event. V. the Infrared Decline

TL;DR

This paper suggests that the near-infrared decline during Eta Carinae's spectroscopic event is caused by accreted mass blocking the secondary star's radiation, reducing dust heating, with pre-event IR increase due to hot dust formation in wind collision zones.

Contribution

It introduces an accretion-based model explaining IR flux variations during Eta Carinae's spectroscopic events, emphasizing dust formation and radiation blocking mechanisms.

Findings

IR decline correlates with accretion phase blocking secondary radiation.

Pre-event IR increase linked to hot dust formation in wind collision region.

Model explains IR behavior during periastron passages.

Abstract

We propose that the decline in the near-IR flux from the massive binary system Eta Carinae during the spectroscopic event might be explained by accreted mass that absorbs the radiation from the secondary star, and by that reduces the heating of the dust that is responsible for the near-IR emission. This binary system has an orbital period of 2024 days and eccentricity of e~0.9. The emission in several bands declines for several weeks near every periastron passages, in what is termed the spectroscopic event. In the accretion model for the spectroscopic event the secondary star accretes mass from the primary's wind for ~10 weeks near every periastron passage. The mass is accreted mainly in the equatorial plane. The disk and its wind block the secondary's radiation from heating dust that does not reside within narrow cones along the symmetry axis. This, we propose, might explain the decline in the near-IR flux occurring at the beginning of each spectroscopic event. We also argue that the increase in the near-IR prior to the event might be accounted for by enhanced hot (T~1700 K) dust formation in the collision region of the winds from the two stars. This dust resides within ~60 degrees from the equatorial plane, and most of it cannot be heated by the secondary during the accretion phase.