Numerical modeling of the bipolar outflows of Eta-Carinae

Details Numerical modeling of the bipolar outflows of Eta-Carinae Numerical modeling of the bipolar outflows of Eta-Carinae

Aug 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003basbr..23..220g&link_type=abstract

Boletim da Sociedade Astronômica Brasileira (ISSN 0101-3440), vol.23, no.1, p. 220-220

Mathematics

Logic

Scientific paper

We present 2-D gas dynamics simulations of the formation and evolution of the supermassive star system η-Carinae bipolar outflows (the homunculus). We investigate the colliding wind scenario under the light of high-resolution numerical simulations. For this aim, we have employed a version of the hydrodynamical adaptative grid-based code Yguazu-A (developed by Raga et al. 2000). We have adopted a colliding stellar wind model (e.g. Frank et al. 1995) where a high velocity outflow interacts with a low-speed one previously ejected. In order to estimate some free parameters of the model and carry out the numerical simulations, we have used kinematical properties recently observed in the homunculus. We find that the observed morphological structure is best reproduced by a model where both the slow and fast winds are anisotropically ejected from the star with initial angular density and velocity distributions (probably produced by source rotation). On the other hand, in a model where the fast wind blows out initially isotropically into the anisotropic slow wind previously ejected, the fast wind tends to sweep out the homunculus structure and isotropize the medium. Presently, we have in progress simulations of interacting winds with distinct degrees of anisotropy to examine the simultaneous formation of the homunculus structure and the equatorial ejection.

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