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G-type main-sequence star

The Sun, a typical example of a G-type main-sequence star

A G-type main-sequence star (spectral type: G-V), also often, and imprecisely, called a yellow dwarf, or G star, is a main-sequence star (luminosity class V) of spectral type G. Such a star has about 0.9 to 1.1 solar masses and an effective temperature between about 5,300 and 6,000 K (5,000 and 5,700 °C; 9,100 and 10,000 °F). Like other main-sequence stars, a G-type main-sequence star converts the element hydrogen to helium in its core by means of nuclear fusion. The Sun, the star in the center of the Solar System to which the Earth is gravitationally bound, is an example of a G-type main-sequence star (G2V type). Each second, the Sun fuses approximately 600 million tons of hydrogen into helium in a process known as the proton–proton chain (4 hydrogens form 1 helium), converting about 4 million tons of matter to energy.[1][2] Besides the Sun, other well-known examples of G-type main-sequence stars include Alpha Centauri, Tau Ceti, and 51 Pegasi.[3][4][5][6]

Description

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The term yellow dwarf is a misnomer, because G-type stars actually range in color from white, for more luminous types like the Sun, to only very slightly yellowish for less massive and luminous G-type main-sequence stars.[7] The Sun is in fact white, but it can often appear yellow, orange or red through Earth's atmosphere due to atmospheric Rayleigh scattering, especially at sunrise and sunset.[8][9][10] In addition, although the term "dwarf" is used to contrast G-type main-sequence stars with giant stars or bigger, stars similar to the Sun still outshine 90% of the stars in the Milky Way (which are largely much dimmer orange dwarfs, red dwarfs, and white dwarfs which are much more common, the latter being stellar remnants).[11]

A G-type main-sequence star with the mass of the Sun will fuse hydrogen for approximately 10 billion years, until the hydrogen element is exhausted at the center of the star. When this happens, the star rapidly expands, cooling and darkening as it passes through the subgiant branch and ultimately expanding into many times its previous size at the tip of the red giant phase, about 1 billion years after leaving the main sequence. After this, the star's degenerate helium core abruptly ignites in a helium flash fusing helium, and the star passes on to the horizontal branch, and then to the asymptotic giant branch. Expanding even further as helium starts running out as it pulses violently, the star's gravity is not sufficient to hold its outer envelope, resulting in significant mass loss and shedding. The ejected material remains as a planetary nebula, radiating as it absorbs energetic photons from the photosphere. Eventually, the core begins to fade as nuclear reactions cease, and becomes a dense, compact white dwarf, which cools slowly from its high initial temperature as the nebula fades.[12][13]

Spectral standard stars

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Properties of typical G-type main-sequence stars[14][15]
Spectral
type 		Mass (M☉) Radius (R☉) Luminosity (L☉) Effective
temperature
(K) 		Color
index
(B − V)
G0V 1.06 1.100 1.35 5,930 0.60
G1V 1.03 1.060 1.20 5,860 0.62
G2V 1.00 1.012 1.02 5,770 0.65
G3V 0.99 1.002 0.98 5,720 0.66
G4V 0.985 0.991 0.91 5,680 0.67
G5V 0.98 0.977 0.89 5,660 0.68
G6V 0.97 0.949 0.79 5,600 0.70
G7V 0.95 0.927 0.74 5,550 0.71
G8V 0.94 0.914 0.68 5,480 0.73
G9V 0.90 0.853 0.55 5,380 0.78

The revised Yerkes Atlas system (Johnson & Morgan 1953)[16] listed 11 G-type dwarf spectral standard stars; however, not all of these still exactly conform to this designation.

The "anchor points" of the MK spectral classification system among the G-type main-sequence dwarf stars, i.e. those standard stars that have remained unchanged over years, are Chara (G0V), the Sun (G2V), Kappa1 Ceti (G5V), 61 Ursae Majoris (G8V).[17] Other primary MK standard stars include HD 115043 (G1V) and 16 Cygni B (G3V).[18] The choices of G4 and G6 dwarf standards have changed slightly over the years among expert classifiers, but often-used examples include 70 Virginis (G4V) and 82 Eridani (G6V). There are not yet any generally agreed upon G7V and G9V standards.

Habitability

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Main article: Habitability of yellow dwarf systems

G-type main sequence stars can provide habitability for life to develop, such as the Sun with life on Earth.[19] They also live long enough to give life enough time to develop, between 7.9 and 13 billion years. Our Sun’s lifetime is about 10 billion years.[20]

Planets

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Besides the Sun and its planets, some of the nearest G-type stars known to have planets include 61 Virginis, HD 102365, HD 147513, Chalawan, Cervantes and Tau Ceti.

See also

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References

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  1. ^ "Why Does The Sun Shine?" Archived 2006-09-09 at the Wayback Machine, lecture, Barbara Ryden, Astronomy 162, Ohio State University, accessed on line June 19, 2007.
  2. ^ "Sun" Archived 2007-06-16 at the Wayback Machine, entry at ARICNS, accessed June 19, 2007.
  3. ^ "Alpha Centauri A" Archived 2019-04-28 at the Wayback Machine, SIMBAD query result. Accessed on line December 4, 2007.
  4. ^ "Tau Ceti" Archived 2019-04-28 at the Wayback Machine, SIMBAD query result. Accessed on line December 4, 2007.
  5. ^ "51 Pegasi" Archived 2019-04-28 at the Wayback Machine, SIMBAD query result. Accessed December 4, 2007.
  6. ^ "Type G Stars". www.whillyard.com. Retrieved 2022-04-22.
  7. ^ What Color Are the Stars? Archived 2017-08-06 at the Wayback Machine, Mitchell N. Charity's webpage, accessed November 25, 2007
  8. ^ Cain, Frazer. "WHAT COLOR IS THE SUN?". Universe Today. Archived from the original on 2012-03-20. Retrieved 2017-11-06.
  9. ^ "What Color is the Sun?". Stanford University. Archived from the original on 2017-10-30. Retrieved 2017-11-06.
  10. ^ Dissanaike, George (19 October 1991). "Painting the sky red". New Scientist. 132 (1791): 31–33.
  11. ^ "More G Stars | StarDate Online". stardate.org. Retrieved 2022-04-22.
  12. ^ Hurley, J. R.; Pols, O. R.; Tout, C. A. (1 July 2000). "Comprehensive analytic formulae for stellar evolution as a function of mass and metallicity". Monthly Notices of the Royal Astronomical Society. 315 (3): 543–569. arXiv:astro-ph/0001295. Bibcode:2000MNRAS.315..543H. doi:10.1046/j.1365-8711.2000.03426.x. S2CID 18523597.
  13. ^ "Evolution from the Main Sequence to Red Giants | Astronomy". courses.lumenlearning.com. Retrieved 2022-04-22.
  14. ^ Pecaut, Mark J.; Mamajek, Eric E. (1 September 2013). "Intrinsic Colors, Temperatures, and Bolometric Corrections of Pre-main-sequence Stars". The Astrophysical Journal Supplement Series. 208 (1): 9. arXiv:1307.2657. Bibcode:2013ApJS..208....9P. doi:10.1088/0067-0049/208/1/9. ISSN 0067-0049. S2CID 119308564.
  15. ^ Mamajek, Eric (2 March 2021). "A Modern Mean Dwarf Stellar Color and Effective Temperature Sequence". University of Rochester, Department of Physics and Astronomy. Retrieved 5 July 2021.
  16. ^ Fundamental stellar photometry for standards of spectral type on the revised system of the Yerkes spectral atlas Archived 2019-04-02 at the Wayback Machine H.L. Johnson & W.W. Morgan, 1953, Astrophysical Journal, 117, 313
  17. ^ MK ANCHOR POINTS Archived 2019-06-25 at the Wayback Machine, Robert F. Garrison
  18. ^ The Perkins Catalog of Revised MK Types for the Cooler Stars Archived 2017-10-11 at the Wayback Machine, P.C. Keenan & R.C McNeil, "Astrophysical Journal Supplement Series" 71 (October 1989), pp. 245–266.
  19. ^ Mullen, Leslie (18 May 2001). "Galactic Habitable Zones". Astrobiology Magazine. Archived from the original on 7 August 2011. Retrieved 1 June 2020.
  20. ^ "Stellar Lifetimes". hyperphysics.phy-astr.gsu.edu. Retrieved 2024-07-20.
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Media related to Yellow dwarfs at Wikimedia Commons