Statistics – Computation
Scientific paper
Nov 1979
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979a%26a....80...97r&link_type=abstract
Astronomy and Astrophysics, vol. 80, no. 1, Nov. 1979, p. 97-103.
Statistics
Computation
60
Mass Flow Rate, Novae, Stellar Envelopes, Stellar Mass Ejection, Stellar Winds, Transonic Flow, Adiabatic Flow, Computational Fluid Dynamics, Energy Budgets, Photosphere, Steady State, Stellar Luminosity, Stellar Models, Supersonic Flow, White Dwarf Stars
Scientific paper
A numerical study is presented of the structure of steady-state optically thick wind models from the critical point out to the photosphere. The evolution of novae during decline is treated as a quasi-stationary sequence of such models. It is found that the photospheric luminosity in all cases must be very close to the Eddington value of approximately 10 to the 38th erg/sec, providing a natural explanation for the observed constancy of the bolometric luminosity at about the Eddington luminosity during the early stages of the decline of novae. Assuming radiative diffusion, the flow is found to be essentially adiabatic deep below the photosphere and in the region of the critical point, but the small deviations from adiabatic flow are crucial in determining the transonic structure. When sequences of models are considered it is found that only those with a critical radius very near to the white dwarf surface reproduce observed outflow velocities, implying that the mechanisms giving rise to the nova outburst are primarily associated with the white dwarf component.
Bath Geoffrey T.
Ruggles Clive L. N.
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