Astronomy and Astrophysics – Astrophysics
Scientific paper
Oct 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...297..455f&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 297, Oct. 15, 1985, p. 455-475.
Astronomy and Astrophysics
Astrophysics
48
Mira Variables, Shock Wave Propagation, Stellar Atmospheres, Stellar Models, Variable Stars, Balmer Series, Emission Spectra, Hydrogen Atoms
Scientific paper
Models of the structure of shock waves in the outer layers of Mira variables are described along with the resultant Balmer line fluxes. The effect of varying preshock density, preshock temperature, and speed of the shock relative to the preshock material is considered, and the role played by molecular hydrogen is studied. Adopting a preshock density estimate of about 5 x 10 to the -11th g/cu cm, the present models predict levels of Balmer emission near maximum light which are much brighter than observed levels, and they predict line ratios generally similar to those of pure recombination, contrary to the observational values. Balmer line fluxes, line profiles, and line ratios in better agreement with observations are obtained if the adopted preshock densities are reduced by a factor of about ten. Estimates of shock propagation velocity in the outer layers of Mira variables are made. A typical shock is expected to decelerate from about 30 km/s at maximum light to about 20 km/s at phase 0.25.
Fox Matthew W.
Wood Peter R.
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