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Modeling hydrogen-deficient Planetary Nebulae

Published online by Cambridge University Press:  25 May 2016

J. P. Harrington ,
K. J. Borkowski  and
Z. I. Tsvetanov
J. P. Harrington
Affiliation:
1U. of Maryland
K. J. Borkowski
Affiliation:
2North Carolina State U.
Z. I. Tsvetanov
Affiliation:
3Johns Hopkins U.

Extract

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Hydrogen-deficient planetary nebulae have central regions devoid of hydrogen. (See Harrington 1996 for a review of these nebulae.) They are characterized by exceptionally strong collisionally excited lines of [O III] and [Ne III], but relatively weak or undetected recombination lines of He or other elements. Such nebulae cannot be modeled successfully unless we include some source of heating in addition to photoionization by the central star.

Type
IV. Envelopes
Information
Symposium - International Astronomical Union , Volume 180: Planetary Nebulae , 1997 , pp. 235
Copyright
Copyright © Kluwer 1997 

References

Borkowski, K.J. & Harrington, J.P. 1991, ApJ, 379, 168.Google Scholar
Borkowski, K.J., Harrington, J.P, Blair, W.P., & Bregman, J.D. 1994, ApJ, 435, 722.Google Scholar
Harrington, J.P. 1996, in Hydrogen-Deficient Stars, eds. Jeffery, C.S. and Heber, U., A.P.S. Conf. Ser. No. 96, p. 193.Google Scholar