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EspañolG V STAR
(Redirected from Yellow dwarf)
In astronomy, a 'G V star' is a main-sequence star of spectral type G and luminosity class V. Such a star, which can also be called a 'yellow dwarf', is small (about 0.8 to 1.0 solar masses) and has a surface temperature of between 5,300 and 6,000 K.[1], Tables VII, VIII. Like other main-sequence stars, a G V star is in the process of converting hydrogen to helium in its core by means of nuclear fusion.[2] Our Sun is the most well-known (and most visible) example of a G V star. Each second, it fuses approximately 600 million tons of hydrogen to helium, converting about 4 million tons of matter to energy.[3][4]
A G V star will fuse hydrogen for, very approximately, 10 billion years, until it is exhausted at the center of the star. When this happens, the star expands to many times its previous size and becomes a red giant, such as Aldebaran (Alpha Tauri.)[5] Eventually the red giant sheds its outer layers of gas, which become a planetary nebula, while the core cools and contracts into a small, dense white dwarf.2
1. Empirical bolometric corrections for the main-sequence, G. M. H. J. Habets and J. R. W. Heintze, ''Astronomy and Astrophysics Supplement'' '46' (November 1981), pp. 193–237.
2. Stellar Evolution: Main Sequence to Giant, class notes, Astronomy 101, Valparaiso University, accessed on line June 19, 2007.
3. Why Does The Sun Shine?, lecture, Barbara Ryden, Astronomy 162, Ohio State University, accessed on line June 19, 2007.
4. Sun, entry at ARICNS, accessed June 19, 2007.
5. SIMBAD, entry for Aldebaran, accessed on line June 19, 2007.
★ Star Types at Enchanted Learning.
★ Solar twin
★ Red dwarf
★ Brown dwarf
★ K V star
The Sun, a typical example of a G V star
In astronomy, a 'G V star' is a main-sequence star of spectral type G and luminosity class V. Such a star, which can also be called a 'yellow dwarf', is small (about 0.8 to 1.0 solar masses) and has a surface temperature of between 5,300 and 6,000 K.[1], Tables VII, VIII. Like other main-sequence stars, a G V star is in the process of converting hydrogen to helium in its core by means of nuclear fusion.[2] Our Sun is the most well-known (and most visible) example of a G V star. Each second, it fuses approximately 600 million tons of hydrogen to helium, converting about 4 million tons of matter to energy.[3][4]
A G V star will fuse hydrogen for, very approximately, 10 billion years, until it is exhausted at the center of the star. When this happens, the star expands to many times its previous size and becomes a red giant, such as Aldebaran (Alpha Tauri.)[5] Eventually the red giant sheds its outer layers of gas, which become a planetary nebula, while the core cools and contracts into a small, dense white dwarf.2
| Contents |
| References |
| External link |
| See also |
References
1. Empirical bolometric corrections for the main-sequence, G. M. H. J. Habets and J. R. W. Heintze, ''Astronomy and Astrophysics Supplement'' '46' (November 1981), pp. 193–237.
2. Stellar Evolution: Main Sequence to Giant, class notes, Astronomy 101, Valparaiso University, accessed on line June 19, 2007.
3. Why Does The Sun Shine?, lecture, Barbara Ryden, Astronomy 162, Ohio State University, accessed on line June 19, 2007.
4. Sun, entry at ARICNS, accessed June 19, 2007.
5. SIMBAD, entry for Aldebaran, accessed on line June 19, 2007.
External link
★ Star Types at Enchanted Learning.
See also
★ Solar twin
★ Red dwarf
★ Brown dwarf
★ K V star
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