Statistical evolutionary properties of planetary nebulae Thicknesses of the nebulae and temperatures of the stars

Details Statistical evolutionary properties of planetary nebulae Thicknesses of the nebulae and temperatures of the stars Statistical evolutionary properties of planetary nebulae Thicknesses of the nebulae and temperatures of the stars

May 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986a%26a...160...31s&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 160, no. 1, May 1986, p. 31-38. CNR-supported research.

Astronomy and Astrophysics

Astrophysics

26

Optical Thickness, Planetary Nebulae, Statistical Analysis, Stellar Evolution, Stellar Temperature, Astronomical Spectroscopy, Black Body Radiation, Helium Ions, Spatial Distribution, Stellar Mass, Tables (Data)

Scientific paper

A comparative study of Zanstra temperatures of the central stars of planetary nebulae indicates that when present the discrepancies between TZ H I and TZ He II can be mainly ascribed to the variation of the optical thickness of a nebulae of hydrogen and helium ionized by a star which emits as a black-body. Different evolutionary trends of TZ H I and TZ He II are obtained for planetary nebulae of the subclasses B and C of Greig (1971, 1972): B nebulae spend most of their life in a thick status, whereas C nebulae start as thick objects but they quickly become optically thin. These results give further support to the suggestion by Sabbadin (1984) that planetary nebulae of the subclass B have stellar masses and/or nebular masses which are statistically larger than those of planetary nebulae belonging to the subclass C.

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