Computer Science
Scientific paper
May 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986s%26t....71..450k&link_type=abstract
Sky and Telescope (ISSN 0037-6604), vol. 71, May 1986, p. 450-454.
Computer Science
Dwarf Stars, M Stars, Stellar Evolution, Supergiant Stars, Cool Stars, Stellar Mass Ejection, Stellar Spectra
Scientific paper
The vast differences among the stars are revealed most dramatically by those of spectral class M, the coolest spectral type. The brightest of these red objects are 50 billion times more luminous than the dimmest. The giants are rare and ephemeral; within 10 to 100 million years, they will change into white dwarfs or, perhaps, neutron stars. In contrast, the main sequence M dwarfs are tiny, possessing feeble luminosities resulting from slow rates of energy production. Molecular features give M spectra their characteristic appearance, though atomic lines are also common. Cool stars can be divided into two groups, oxygen- or carbon-rich. The properties of giants and supergiants are discussed in detail, with particular emphasis on mass loss. The most mass loss takes place in the red giant and supergiant realms of the H-R diagram because these stars have very low escape velocities. Through this mass loss, a new mix of elements enters the interstellar medium out of which new stars are created. In contrast to these supergiants, M dwarfs can live for a trillion years, and in effect compose about 90 percent of all stars and about half the stellar mass of the Galaxy.
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