G-type main-sequence star

A G-type main-sequence star (Spectral type: G-V), often 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. Like other main-sequence stars, a G-type main-sequence star is converting the element hydrogen to helium in its core by means of nuclear fusion. The Sun, the star to which the Earth is gravitationally bound in the Solar System, 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 A, Tau Ceti, and 51 Pegasi.[3][4][5]

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

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 yellow for the less massive and luminous G-type main-sequence stars.[6] 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.[7][8][9] In addition, although the term "dwarf" is used to contrast yellow main-sequence stars with giant stars, yellow dwarfs like the Sun outshine 90% of the stars in the Milky Way (which are largely much dimmer orange dwarfs, red dwarfs, and white dwarfs, the latter being stellar remnants).

A G-type main-sequence star will fuse hydrogen for approximately 10 billion years, until it is exhausted at the center of the star. When this happens, the star rapidly expands, cooling as it passes through the subgiant branch and ultimately expanding to 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, and the star passes on to the horizontal branch, and then to the asymptotic giant branch. Expanding even further as it pulses violently, the star's gravity is not sufficient to hold its outer envelope, resulting in significant mass loss. 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.[10]

Spectral standard starsEdit

Properties of typical G-type main-sequence stars[11][12]
Spectral
type
Mass (M) Luminosity (L) Effective
temperature

(K)
Color
index

(B − V)
G0V 1.06 1.35 5,930 0.60
G1V 1.03 1.20 5,860 0.62
G2V 1.00 1.02 5,770 0.65
G3V 0.99 0.98 5,720 0.66
G4V 0.985 0.91 5,680 0.67
G5V 0.98 0.89 5,660 0.68
G6V 0.97 0.79 5,600 0.70
G7V 0.95 0.74 5,550 0.71
G8V 0.94 0.68 5,480 0.73
G9V 0.9 0.55 5,380 0.78

The revised Yerkes Atlas system (Johnson & Morgan 1953)[13] listed 11 G-type dwarf spectral standard stars; however, not all of these still 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 beta CVn (G0V), the Sun (G2V), Kappa1 Ceti (G5V), 61 Ursae Majoris (G8V).[14] Other primary MK standard stars include HD 115043 (G1V) and 16 Cygni B (G3V).[15] 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 (G8V). There are not yet any generally agreed upon G7V and G9V standards.

PlanetsEdit

Besides the sun, some of the nearest G-type stars known to have planets include 61 Virginis, HD 102365, HD 147513, 47 Ursae Majoris, Mu Arae, and Tau Ceti.

See alsoEdit

ReferencesEdit

  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 on line December 4, 2007.
  6. ^ What Color Are the Stars? Archived 2017-08-06 at the Wayback Machine, Mitchell N. Charity's webpage, accessed November 25, 2007
  7. ^ Cain, Frazer. "WHAT COLOR IS THE SUN?". Universe Today. Archived from the original on 2012-03-20. Retrieved 2017-11-06.
  8. ^ "What Color is the Sun?". Stanford University. Archived from the original on 2017-10-30. Retrieved 2017-11-06.
  9. ^ Dissanaike, George (19 October 1991). "Painting the sky red". New Scientist. 132 (1791): 31–33.
  10. ^ 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. doi:10.1046/j.1365-8711.2000.03426.x.
  11. ^ 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: 9. arXiv:1307.2657. doi:10.1088/0067-0049/208/1/9. ISSN 0067-0049.
  12. ^ 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.
  13. ^ 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
  14. ^ MK ANCHOR POINTS Archived 2019-06-25 at the Wayback Machine, Robert F. Garrison
  15. ^ 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.

External linksEdit

  Media related to Yellow dwarfs at Wikimedia Commons