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In 1926, in his book The Internal Constitution of the Stars he explained the physics of how stars fit on the diagram. [15] The paper anticipated the later discovery of nuclear fusion and correctly proposed that the star's source of power was the combination of hydrogen into helium, liberating enormous energy.
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Stars less massive than 0.25 M ☉, called red dwarfs, are able to fuse nearly all of their mass while stars of about 1 M ☉ can only fuse about 10% of their mass. The combination of their slow fuel-consumption and relatively large usable fuel supply allows low mass stars to last about one trillion ( 10 × 10 12 ) years; the most extreme of 0. ...
The Stars: A New Way to See Them is an astronomy book by H. A. Rey. It was first published in 1952 (Houghton Mifflin, Boston) and revised in 1962. It was updated again in 1997. Other editions were: Chatto and Windus, London, 1975; "A New Way to see the Stars", Paul Hamlyn, London, 1966; Enl. World-wide ed. Houghton Mifflin, 1967.
O-type stars are very hot and extremely luminous, with most of their radiated output in the ultraviolet range. These are the rarest of all main-sequence stars. About 1 in 3,000,000 (0.00003%) of the main-sequence stars in the solar neighborhood are O-type stars. [c] [11] Some of the most massive stars lie within this spectral class. O-type ...
A characteristic of population II stars is that despite their lower overall metallicity, they often have a higher ratio of alpha elements (elements produced by the alpha process, like oxygen and neon) relative to iron (Fe) as compared with population I stars; current theory suggests that this is the result of type II supernovas being more ...
A-type star In the Harvard spectral classification system, a class of main-sequence star having spectra dominated by Balmer absorption lines of hydrogen. Stars of spectral class A are typically blue-white or white in color, measure between 1.4 and 2.1 times the mass of the Sun, and have surface temperatures of 7,600–10,000 kelvin.
Stars may also pulsate in a harmonic or overtone which is a higher frequency, corresponding to a shorter period. Pulsating variable stars sometimes have a single well-defined period, but often they pulsate simultaneously with multiple frequencies and complex analysis is required to determine the separate interfering periods.