On the structural development of the shells of novae and planetary nebulae

Details On the structural development of the shells of novae and planetary nebulae On the structural development of the shells of novae and planetary nebulae

Jul 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977a%26a....59...91p&link_type=abstract

Astronomy and Astrophysics, vol. 59, no. 1, July 1977, p. 91-110.

Astronomy and Astrophysics

Astrophysics

55

Astronomical Models, Novae, Planetary Nebulae, Stellar Models, Astrophysics, Gravitational Effects, Radiation Pressure

Scientific paper

The structural development of nebular shells is investigated using a model in which gravitational braking, radiation pressure, and stellar rotation are responsible for the ultimate nebular forms. It is assumed that mass is ejected from the central star with sufficient energy to escape, and models for the ejection process are considered which involve either instantaneous ejection at a range of velocities, gradual ejection at a unique velocity, or instantaneous ejection at a unique velocity. Effects of gravitational braking, Lyman-continuum radiation pressure, and stellar rotation on terminal shell configurations are analyzed in detail, and a full range of possible nebular shapes is generated, including toroids, ellipsoids, and hour glasses. A simple theory of radiative acceleration is developed, the basic configurations obtained are compared with representative nebulae, and the development of the shell of Nova DQ Her is examined. It is concluded that the most commonly observed nebular shapes as well as some less common forms can be readily accounted for in the framework of the model employed.

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