Other
Scientific paper
Jan 1982
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982s%26w....21...17k&link_type=abstract
Sterne und Weltraum, vol. 21, Jan. 1982, p. 17-20. In German.
Other
O Stars, Planetary Nebulae, Stellar Evolution, Stellar Spectra, Subdwarf Stars, White Dwarf Stars, Asymptotic Giant Branch Stars, Asymptotic Methods, Mass Distribution, Spectrum Analysis, Statistical Analysis, Stellar Luminosity, Stellar Mass
Scientific paper
Central stars of planetary nebulae (CSPN) and subdwarf O stars (sdO) have similar spectra and are comparable in radius, mass, and luminosity. The main difference between CSPN and sdO is that the former are surrounded by a characteristic nebula, while the latter have no sign of clouds. Using the theory of stellar evolution, a genetic relation between white dwarfs, CSPN and sdO is established. The mass distribution of white dwarfs and CSPN is analyzed statistically, showing that the latter, in contrast to the former, have no star with a mass less than 0.55 solar mass. A diagram of gravity versus effective temperature is also given for sdO stars and CSPN. The sdO stars are shown to have too low a mass to expand to red giants and are considered to be low-mass precursors of white dwarfs; CSPN, on the other hand, reach the asymptotic giant branch because of their originally high mass and form clouds. They are considered the high-mass precursors of white dwarfs.
No associations
LandOfFree
Central stars of planetary nebulae and subdwarf O stars does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Central stars of planetary nebulae and subdwarf O stars, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Central stars of planetary nebulae and subdwarf O stars will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1458184