Astronomy and Astrophysics – Astrophysics
Scientific paper
Jun 1989
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989a%26a...216..245z&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 216, no. 1-2, June 1989, p. 245-252. Research supported by ZWO.
Astronomy and Astrophysics
Astrophysics
41
Galactic Nuclei, Planetary Nebulae, Stellar Evolution, Stellar Mass, Asymptotic Giant Branch Stars, H Beta Line, Optical Thickness, Stellar Luminosity, Stellar Temperature, Very Large Array (Vla)
Scientific paper
A group of weak, low-excitation planetary nebulae in the galactic bulge are studied. The properties of the nebulae are within the normal range for planetary nebulae, but some have a very low total ionized mass. From the observed properties of the nebulae the temperatures of the central stars are estimated. With two possible exceptions, the stars have not yet entered the cooling track in the HR diagram. It is shown that, if the planetary nebulae are optically thick to the ionizing stellar radiation, the total luminosity can be derived from the H-beta luminosity in a way analogous to the Zanstra (1931) method for determining stellar temperatures. The resulting position in the HR diagram is in most cases not consistent with the theoretically predicted evolutionary tracks. Thus, the nebulae may be optically thin, in spite of the very low mass of some of the objects.
Pottasch Stuart R.
Zijlstra Albert A.
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