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Nova Models and their Problems

Published online by Cambridge University Press:  12 April 2016

H.-C. Thomas
H.-C. Thomas*
Affiliation:
Max-Planck-Institut für Physik und Astrophysik, Föhringer Ring 6, 8000 München 40, FRG

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Very detailed spectroscopic and photometric observations of Novae are available today. Unfortunately they do not directly tell us what suddenly makes a star a million times brighter, sometimes even transforming the familiar constellations on the sky. Twenty-five years after its publication, Mestel’s (1952) metaphor of a gigantic hydrogen bomb seems to be most widely accepted, although he at that time applied his model to a Supernova outburst. Later Giannone and Weigert (1967) as well as Rose (1968), Saslaw (1968) and others have computed hydrostatic models of such an event, using Kraft’s (1963) binary model of a late type main sequence star and a white dwarf. Detailed hydrodynamic computations were carried out by Starrfield and his collaborators (for references see Sparks, Starrfield, and Truran, 1977) and recently by Prialnik, Shara, and Shaviv (A & A 62, 339, 1978).

Type
Part II: Cataclysmic Variables
Information
International Astronomical Union Colloquium , Volume 42: The Interaction of Variable Stars with their Environment , 1977 , pp. 301 - 310
Copyright
Copyright © Veröff. Der Remeis-Sterwarte 1977

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