3D Modeling of the Massive Binary Wind Interaction Region in Eta Carinae

Details 3D Modeling of the Massive Binary Wind Interaction Region in Eta Carinae 3D Modeling of the Massive Binary Wind Interaction Region in Eta Carinae

Jan 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21340802m&link_type=abstract

American Astronomical Society, AAS Meeting #213, #408.02; Bulletin of the American Astronomical Society, Vol. 41, p.205

Astronomy and Astrophysics

Astronomy

Scientific paper

We present recent work on the theoretical modeling of low excitation ([Fe II]) and high excitation ([Fe III]) wind lines observed in Eta Carinae using the HST/STIS. The spatially resolved structures seen in these lines are interpreted as the time-averaged, outer extensions of the wind from the primary star and the wind-wind interaction region of the massive binary system. For most of the orbit, the wind-wind interface can be approximated as a cone with a half-opening angle of 65° whose axis of rotation is aligned with the major axis of the binary orbit and appears to lie in the plane of the Homunculus disk. However, because the orbit is highly elliptical, this approximation breaks down at periastron and so full 3D Smoothed Particle Hydrodynamics (SPH) simulations become necessary. By analyzing the results of these 3D SPH simulations of the binary interactions and comparing them to the spectra obtained with the HST/STIS we place further constraints on the orientation of the binary orbit, and hope to eventually determine how/where UV light is escaping in the system, to search for any direct signatures of the companion star, and to ultimately establish a mass ratio for the system.

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