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G-type main-sequence star

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"Yellow dwarf" redirects here. For the fairy tale by Madame d'Aulnoy, see The Yellow Dwarf.
The Sun, a typical example of a G-type main-sequence star.
Properties of typical G-type main-sequence stars[1]
Spectral
type 		Mass (M☉) Surface
gravity
(log g) 		Effective
temperature
(K) 		Color
index
(B − V)
G0V 1.15 4.32 5,980 0.583
G1V 1.10 4.34 5,900 0.608
G2V 1.07 4.35 5,800 0.625
G3V 1.04 4.37 5,710 0.642
G4V 1.00 4.38 5,690 0.657
G5V[note 1] 0.98 4.40 5,620 0.672
G6V 0.93 4.42 5,570 0.690
G7V 0.90 4.44 5,500 0.713
G8V 0.87 4.46 5,450 0.740
G9V 0.84 4.48 5,370 0.776

A G-type main-sequence star (Spectral type: G-V), often (and imprecisely) called a yellow dwarf, or G dwarf star, is a main-sequence star (luminosity class V) of spectral type G. Such a star has about 0.8 to 1.2 solar masses and surface temperature of between 5,300 and 6,000 K.[2], Tables VII, VIII. 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.[3] The Sun, the star to which the Earth is gravitationally bound in the Solar System and the object with the largest apparent magnitude, is an example of a G-type main-sequence star. Each second, the Sun fuses approximately 600 million tons of hydrogen to helium, converting about 4 million tons of matter to energy.[4][5] Besides the Sun, other well-known examples of G-type main-sequence stars include Alpha Centauri A, Tau Ceti, and 51 Pegasi.[6][7][8]

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.[9] The Sun is in fact white, but appears yellow through Earth's atmosphere due to atmospheric Rayleigh scattering.[10] In addition, although the term "dwarf" is used to contrast yellow main-sequence stars from 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 last being a stellar remnant).

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 expands to many times its previous size and becomes a red giant, such as Aldebaran (or Alpha Tauri).[11] Eventually the red giant sheds its outer layers of gas, which become a planetary nebula, while the core rapidly cools and contracts into a compact, dense white dwarf.[3]

Spectral standard stars

The revised Yerkes Atlas system (Johnson & Morgan 1953)[12] listed 11 G-type dwarf spectral standard stars; however, not all of these have survived to this day as standards.

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).[13] Other primary MK standard stars include HD 115043 (G1V) and 16 Cygni B (G3V).[14] 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.

Planets

Some of the nearest G-type stars known to have planets include the Sun, 61 Virginis, HD 102365, HD 147513, 47 Ursae Majoris, Mu Arae, and possibly Alpha Centauri.

See also

Notes

  1. ^ The Sun is not in this class because even though it corresponds to the same mass, the Sun is slightly hotter than the typical temperature for a G5V star (at 5,778 K), so it is a G2V star, which is normally slightly more massive than the Sun

References

  1. ^ Vardavas, Ilias M.; et al. (2011), "Chapter 5. Incoming Solar Radiation", Radiation and Climate: Atmospheric Energy Budget from Satellite Remote Sensing, International Series of Monographs on Physics, vol. 138, OUP Oxford, p. 130, ISBN 0199697140
  2. ^ 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.
  3. ^ a b Stellar Evolution: Main Sequence to Giant, class notes, Astronomy 101, Valparaiso University, accessed on line June 19, 2007.
  4. ^ Why Does The Sun Shine?, lecture, Barbara Ryden, Astronomy 162, Ohio State University, accessed on line June 19, 2007.
  5. ^ Sun, entry at ARICNS, accessed June 19, 2007.
  6. ^ Alpha Centauri A, SIMBAD query result. Accessed on line December 4, 2007.
  7. ^ Tau Ceti, SIMBAD query result. Accessed on line December 4, 2007.
  8. ^ 51 Pegasi, SIMBAD query result. Accessed on line December 4, 2007.
  9. ^ What Color Are the Stars?, Mitchell N. Charity's webpage, accessed November 25, 2007
  10. ^ Dissanaike, George (19 October 1991). "Painting the sky red". New Scientist. 132 (1791): 31–33.
  11. ^ SIMBAD, entry for Aldebaran, accessed on line June 19, 2007.
  12. ^ Fundamental stellar photometry for standards of spectral type on the revised system of the Yerkes spectral atlas H.L. Johnson & W.W. Morgan, 1953, Astrophysical Journal, 117, 313
  13. ^ MK ANCHOR POINTS, Robert F. Garrison
  14. ^ The Perkins Catalog of Revised MK Types for the Cooler Stars, P.C. Keenan & R.C McNeil, "Astrophysical Journal Supplement Series" 71 (October 1989), pp. 245–266.

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