Hydrodynamic Simulations of H alpha Emission in Algol-Type Binaries

Details Hydrodynamic Simulations of H alpha Emission in Algol-Type Binaries Hydrodynamic Simulations of H alpha Emission in Algol-Type Binaries

Jan 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998apj...493..326r&link_type=abstract

Astrophysical Journal v.493, p.326

Astronomy and Astrophysics

Astronomy

29

Accretion, Accretion Disks, Stars: Binaries: Eclipsing, Stars: Circumstellar Matter, Hydrodynamics, Stars: Imaging, Stars: Individual Constellation Name: Tt Hydrae, Stars: Individual Constellation Name: Beta Persei, Stars: Individual Constellation Name: U Coronae Borealis, Stars: Individual Constellation Name: U Sagittae, Stars: Individual Constellation Name: V711 Tauri

Scientific paper

Two-dimensional hydrodynamic simulations of mass transfer in short-period Algol-type binaries were performed using the numerical code Virginia Hydrodynamics 1. This code uses the piecewise parabolic method with a Lagrangian remap. Our version of the code also accounts for radiative cooling and collisional ionization and excitation processes. The purpose of performing the simulations was to study the H alpha emission from circumstellar gas in the Algols. Using observational evidence from the literature to constrain the gas stream properties, hydrodynamic maps of the H alpha emissivity in the two systems beta Per (P = 2.87 days) and TT Hya (P = 6.95 days) were made in both Cartesian and velocity coordinates from the simulation data. The velocity maps were then compared to Doppler tomograms constructed from observed H alpha line emission in these systems. Since the tomograms cannot be directly transformed to maps of emission in spatial coordinates, the simulated Cartesian maps enabled us to interpret the dynamical processes that produce the features observed in the Doppler tomograms. We find that the simulations produce asymmetric accretion structures with many features similar to those found in the Doppler tomograms of Algol systems.

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