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Internal Kinematics of the Planetary Nebulae

Published online by Cambridge University Press:  03 August 2017

O. C. Wilson
O. C. Wilson*
Affiliation:
Mount Wilson and Palomar Observatories, Carnegie Institution of Washington, and California Institute of Technology, Pasadena, California

Extract

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A common form of planetary nebula consists of a high temperature nuclear star surrounded by an ovoid or ellipsoidal shell of gas which has originated in some manner in the nucleus. The radiation from the nebula consists of the ordinary spectral lines and continua of hydrogen and helium plus the so-called forbidden lines of atoms and ions of oxygen, nitrogen, neon, argon, etc. It has become clear that, as in other cosmic bodies, the bulk of the nebula consists of hydrogen and helium, and the remainder of the chemical elements occur only as a slight admixture of impurities. For instance, recent data by Aller and Minkowski lead to relative numbers of atoms of various chemical species in a particular nebula (NGC 7027) as follows (oxygen arbitrarily taken as 104):

Type
Part V: Kinematic Structure of Gaseous Envelopes
Information
Symposium - International Astronomical Union , Volume 8: Cosmical Gas Dynamics , July 1958 , pp. 1025 - 1029
Copyright
Copyright © American Physical Society 1958 

References

1 Aller, L. H. and Minkowski, R., Astrophys. J. 124, 110 (1956).Google Scholar

2 Milne, E. A., Z. Astrophys. 1, 98 (1930).Google Scholar