The upper end of the main series

Details The upper end of the main series The upper end of the main series

Apr 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983s%26w....22..179s&link_type=abstract

Sterne und Weltraum (ISSN 0039-1263), vol. 22, April 1983, p. 179-181. In German.

Physics

Hertzsprung-Russell Diagram, Main Sequence Stars, O Stars, Stellar Luminosity, Stellar Mass, Giant Stars, Stellar Evolution, Stellar Mass Ejection

Scientific paper

Attention is given to stars with the greatest absolute brightness, taking into account questions regarding a limitation of the main series with respect to large luminosities. The spectral classification for the class O is considered. It is found that the earliest O stars, such as O3 to O5 can have a greater absolute brightness as the brightest supergiants of a later spectral type. The largest values of absolute brightness determined for early galactic O stars are approximately M(bol) = -11. The luminosities involved are approximately one million times as large as that of the sun. Lifetime and frequency of the O stars are discussed along with questions of instability and mass loss, the evolutionary path for stars of different mass, arguments that protostars of very large mass cannot reach the main series, and a number of factors which can limit stellar mass.

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