Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...181.1903o&link_type=abstract
American Astronomical Society, 181st AAS Meeting, #19.03; Bulletin of the American Astronomical Society, Vol. 24, p.1150
Astronomy and Astrophysics
Astronomy
Scientific paper
We use a 2-D PPM code to simulate numerically the hydrodynamics of a radiation-driven stellar wind from a rapidly rotating B-star. The results generally confirm predictions of a semi-analytic ``Wind-Compressed-Disk" model recently proposed by Bjorkman and Cassinelli to explain the circumstellar disks inferred observationally to exist around Be stars. However, this numerical simulation is able to incorporate several important effects not accounted for in the simple model, including a dynamical treatment of the outward radiative driving and gas pressure. This enables us to model quantatively the compressed wind and shock that forms the equatorial disk. The simulation results thus do differ in several important details from the simple model, showing, for example, cases of inner disk inflow not possible in the heuristic approach of assuming a fixed outward velocity law. This poster paper will present a detailed comparison of the analytic and numerical models.
Blondin John
Cranmer Steven
Owocki Stanley
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