Wind Bubbles around Massive Stars: Ionization-Gasdynamics Modelling and X-ray Emission Calculations

Details Wind Bubbles around Massive Stars: Ionization-Gasdynamics Modelling and X-ray Emission Calculations Wind Bubbles around Massive Stars: Ionization-Gasdynamics Modelling and X-ray Emission Calculations

Jan 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21725113d&link_type=abstract

American Astronomical Society, AAS Meeting #217, #251.13; Bulletin of the American Astronomical Society, Vol. 43, 2011

Astronomy and Astrophysics

Astrophysics

Scientific paper

Using a code that employs a self-consistent method for computing the effects of photo-ionization on circumstellar gas dynamics, we model the formation of wind-driven nebulae around massive stars. Our algorithm incorporates a simplified model of the photo-ionization source, computes the fractional ionization of hydrogen due to the photo-ionizing flux and recombination, and determines self-consistently the energy balance due to ionization, photo-heating and radiative cooling. We take into account changes in stellar properties and mass-loss over the star's evolution. Our multi-dimensional simulations clearly reveal the presence of strong ionization front instabilities, similar to those seen in galactic ionization fronts. In this poster we describe the code, and show how inclusion of photo-ionization affects the wind bubble structure and dynamics. Using various X-ray emission models, we compute the X-ray flux and spectra from our wind bubble models, and compare to observed data.
VVD's research is supported by grant TM9-0001X provided by NASA through the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060.

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