Shock waves and H-alpha profiles in the hydrodynamical model for RR Lyrae

Details Shock waves and H-alpha profiles in the hydrodynamical model for RR Lyrae Shock waves and H-alpha profiles in the hydrodynamical model for RR Lyrae

May 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992mnras.256...26f&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 256, no. 1, May 1, 1992, p. 26-36.

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34

Astronomical Models, Blue Stars, H Alpha Line, Hydrodynamic Equations, Shock Waves, Variable Stars, Computational Astrophysics, Emission Spectra, Giant Stars, Local Thermodynamic Equilibrium, Shock Fronts, Stellar Oscillations

Scientific paper

The shock phenomena and H-alpha formation in the atmosphere of RR Lyrae are investigated by means of numerical simulations. The H-alpha profiles are obtained by solution of the non-LTE line transfer problem for the multilevel hydrogen atom. A close quantitative agreement between the predicted and observed profiles is found, confirming the adequacy of the model used. In the course of pulsations the model produces an extended atmosphere of about 16 static scaleheights, in which two shocks are successively generated during one period. These results generally confirm the earlier conclusions of Hill. It is suggested that the bump of the light curve is connected with the early shock generation, the mechanism for which is discussed. The full development of the main shock occurs very high in the atmosphere. This can explain both the lack of doubling of the weak metallic lines, formed at a relatively large depth, and the absence of prominent emission in H-alpha due to large deviations from LTE near the shock front. Strong emission in the Lyman lines is predicted, reaching maximum intensity near the light maximum.

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