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The structure and evolution of close binary stars has been studied using the twodimensional (2D) stellar structure algorithm developed by Deupree (1995). We have calculated a series of solar composition stellar evolution sequences of binary models, where the mass of the 2D model is 8M⊙ with a point-mass 5M⊙ companion. We have also studied the structure of… (More)

The possibility of a dynamical core helium Ñash has been studied with two-dimensional hydrodynamic simulations using three separate turbulence models for the treatment of time-dependent convection. Two of these are simple algebraic eddy viscosity models. The third model involves a separate equation for the turbulent kinetic energy density, which then feeds… (More)

Radial and nonradial oscillations offer the opportunity to investigate the interior properties of stars. We use 2D stellar models and a 2D finite difference integration of the linearized pulsation equations to calculate non-radial oscillations. This approach allows us to directly calculate the pulsation modes for a distorted rotating star without treating… (More)

Extreme deformation of a stellar surface, such as that produced by rapid rotation, causes the surface temperature and gravity to vary significantly with latitude. Thus, the spectral energy distribution (SED) of a non-spherical star could differ significantly from the SED of a spherical star with the same average temperature and luminosity. Calculation of… (More)

- C. C. Lovekin, Robert G. Deupree
- 20th International Symposium on High-Performance…
- 2006

We present a method for calculating synthetic line profiles for rapidly rotating, non-spherical stars. This parallel code includes the effects of the Doppler shift produced by the surface rotation, and is capable of simultaneously calculating the observed line profile for several different degrees of inclination between the observer and the star’s… (More)

Extreme deformation of a stellar surface, such as that produced by rapid rotation, causes the surface temperature and gravity to vary significantly with latitude. Thus, the spectral energy distribution (SED) of a non-spherical star could differ significantly from the SED of a spherical star with the same average temperature and luminosity. Calculation of… (More)

- Robert G. Deupree, Patrick Rogers
- 20th International Symposium on High-Performance…
- 2006

The gravitational potential for close binary systems is usually calculated assuming both stars to be point masses. Deupree and Karakas recently examined the internal structure of both members of a binary system under the assumption that the gravitational potential for each member is the gravitational potential produced by its own mass distribution and by a… (More)

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