Astronomy and Astrophysics – Astrophysics
Scientific paper
Feb 1977
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977apj...211..910c&link_type=abstract
Astrophysical Journal, Part 1, vol. 211, Feb. 1, 1977, p. 910-925. Research supported by the Sacramento Peak Observatory;
Astronomy and Astrophysics
Astrophysics
63
Energy Storage, Radiation Pressure, Stellar Atmospheres, Stellar Models, Stellar Winds, Atmospheric Heat Budget, Atmospheric Models, Boltzmann Transport Equation, Flow Stability, Hot Stars, Photosphere, Stellar Interiors, Supersonic Wind Tunnels, Thermodynamic Equilibrium
Scientific paper
Most current models of matter-flux in hot stars place its origin in radiation pressure, and then model the flow explicitly to produce no chromosphere-corona. Our model of the stellar atmosphere as a transition zone between stellar interior and interstellar medium places the origin of matter-flux, chromosphere-corona, and spectral 'emission classes' in subatmospheric nonthermal kinetic energy storage, equally for all stars, hot or cold. Current observations of both hot and cold stars suggest chromospheres to be a universal phenomenon, correlated with matter-fluxes, and enhanced in 'emission-class' stars. To clarify the difference between the two kinds of models above, we reformulate the wind-tunnel analogy to stellar winds, suggesting that stars satisfy an 'imperfect,' rather than 'perfect,' such model; i.e., transonic shocks occur before the throat, corresponding to an imposed outward velocity in the storage section, or subatmosphere. We then investigate the stability of an arbitrary stellar atmosphere, hot or cold, to suggest a cause for such an outward subatmospheric velocity.
Cannon Joseph C.
Thomas Nicholas R.
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