Red dwarf

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This article is about the type of star. For the television sitcom, see Red Dwarf.
Hertzsprung–Russell diagram
Spectral type
Brown dwarfs
White dwarfs
Red dwarfs
Subdwarfs
Main sequence
("dwarfs")
Subgiants
Giants
Bright giants
Supergiants
Hypergiants
absolute
magni-
tude
(MV)

A red dwarf is a small and relatively cool star on the main sequence, either late K or M spectral type. Red dwarfs range in mass from a low of 0.075 solar masses (the upper limit for a brown dwarf) to about 50% of the Sun and have a surface temperature of less than 4,000 K.

Red dwarfs are by far the most common type of star in the Milky Way galaxy, at least in the neighborhood of the Sun, but due to their low luminosity, individual red dwarfs cannot easily be observed. From Earth, not one is visible to the naked eye.[1] Proxima Centauri, the nearest star to the Sun, is a red dwarf (Type M5, apparent magnitude 11.05), as are twenty of the next thirty nearest. According to some estimates, red dwarfs make up three-quarters of the stars in our galaxy.[2]

Stellar models indicate that red dwarfs with less than 35% of the Sun's mass are fully convective.[3] Hence the helium produced by the thermonuclear fusion of hydrogen is constantly remixed throughout the star, avoiding a buildup at the core. Red dwarfs therefore develop very slowly, having a constant luminosity and spectral type for, in theory, some trillions of years, until their fuel is depleted. Because of the comparatively short age of the universe, no red dwarfs of advanced evolutionary stages exist.

Description and characteristics[edit]

Red dwarfs are very-low-mass stars.[4] Consequently they have relatively low temperatures in their cores and energy is generated at a slow rate through nuclear fusion of hydrogen into helium by the proton–proton (PP) chain mechanism. Hence these stars emit little light, sometimes as little as 110,000 that of the Sun. Even the largest red dwarfs (for example HD 179930, HIP 12961 and Lacaille 8760) have only about 10% of the Sun's luminosity.[5] In general, red dwarfs with less than 35% of the Sun's mass transport energy from the core to the surface by convection. Convection occurs because of opacity of the interior, which has a high density compared to the temperature. As a result, energy transfer by radiation is decreased, and instead convection is the main form of energy transport to the surface of the star. Above this mass, the red dwarfs will have a region around their core where convection does not occur.[6]

Typical characteristics[7]
Stellar
class
Mass
(M)
Radius
(R)
Luminosity
(L)
Teff
(K)
M0V 60% 62% 7.2% 3,800
M1V 49% 49% 3.5% 3,600
M2V 44% 44% 2.3% 3,400
M3V 36% 39% 1.5% 3,250
M4V 20% 26% 0.55% 3,100
M5V 14% 20% 0.22% 2,800
M6V 10% 15% 0.09% 2,600
M7V 9% 12% 0.05% 2,500
M8V 8% 11% 0.03% 2,400
M9V 7.5% 8% 0.015% 2,300
The predicted main-sequence lifetime of a red dwarf plotted against its mass relative to the Sun.[8]

As late-type red dwarfs are fully convective, helium does not accumulate at the core and, compared to larger stars such as the Sun, they can burn a larger proportion of their hydrogen before leaving the main sequence. As a result, red dwarfs have estimated lifespans far longer than the present age of the universe, and stars with less than 0.8 solar masses have not had time to leave the main sequence. The lower the mass of a red dwarf, the longer the lifespan. It is believed that the lifespan of these stars exceeds the expected 10 billion year lifespan of our Sun by the third or fourth power of the ratio of the solar mass to their masses; thus a red dwarf with 0.1 solar mass may continue burning for 10 trillion years.[4][9] As the proportion of hydrogen in a red dwarf is consumed, the rate of fusion declines and the core starts to contract. The gravitational energy generated by this size reduction is converted into heat, which is carried throughout the star by convection.[10]

According to computer simulations, the minimum mass a red dwarf must have in order to become a red giant is 0.25 solar masses; less massive objects, as they age, increase their surface temperatures and luminosities becoming blue dwarfs and from that finally become white dwarfs.[8]

The less massive the star, the longer this evolutionary process takes; for example, it has been calculated that a red dwarf with a mass of 0.16 solar masses (approximately the mass of the nearby Barnard's star) would stay on the main sequence during 2.5 trillion years that would be followed by five billion years as blue dwarf, in which the star would have 1/3 of the Sun's luminosity and a surface temperature of 8,500 Kelvin.[8]

The fact that red dwarfs and other low-mass stars remain on the main sequence while more massive stars have moved off the main sequence allows the age of star clusters to be estimated by finding the mass at which the stars turn off the main sequence. This provides a lower, stellar, age limit to the Universe and also allows formation timescales to be placed upon the structures within the Milky Way galaxy, namely the Galactic halo and Galactic disk.

One mystery which has not been solved as of 2009 is the absence of red dwarfs with no metals. (In astronomy, a metal is any element heavier than hydrogen or helium.) The Big Bang model predicts the first generation of stars should have only hydrogen, helium, and trace amounts of lithium. If such stars included red dwarfs, they should still be observable today, but none have yet been identified. The preferred explanation is that without heavy elements only large and not yet observed population III stars can form, and these rapidly burn out, leaving heavy elements which then allow for the formation of red dwarfs. Alternative explanations, such as the idea that zero-metal red dwarfs are dim and could be few in number, are considered much less likely as they seem to conflict with stellar evolution models.

Planets[edit]

Artist's conception of a red dwarf, the most common type of star in the Sun's stellar neighborhood, and in the universe. Although termed a red dwarf, the surface temperature of this star would give it an orange hue when viewed from close proximity

Many red dwarfs are orbited by extrasolar planets but large Jupiter-sized planets are comparatively rare. Doppler surveys around a wide variety of stars indicate about 1 in 6 stars having twice the mass of the Sun are orbited by one or more Jupiter-sized planets, vs. 1 in 16 for Sun-like stars and only 1 in 50 for red dwarfs. On the other hand, microlensing surveys indicate that long-period Neptune-mass planets are found around 1 in 3 red dwarfs. [11] Observations with HARPS further indicate 40% of red dwarfs have a "super-Earth" class planet orbiting in the habitable zone where liquid water can exist on the surface of the planet.[12]

At least four and possibly up to six extrasolar planets were discovered orbiting the red dwarf Gliese 581 between 2005–2010. One planet has about the mass of Neptune, or sixteen Earth masses. It orbits just 6 million kilometers (0.04 AU) from its star, and so is estimated to have a surface temperature of 150 °C, despite the dimness of the star. In 2006, an even smaller extrasolar planet (only 5.5 times the mass of Earth) was found orbiting the red dwarf OGLE-2005-BLG-390L; it lies 390 million km (2.6 AU) from the star and its surface temperature is −220 °C (56 K).

In 2007, a new, potentially habitable extrasolar planet, Gliese 581 c, was found, orbiting Gliese 581. If the minimum mass estimated by its discoverers (a team led by Stephane Udry), namely 5.36 times that of the Earth, is correct, it is the smallest extrasolar planet revolving around a main-sequence star discovered to date and since then Gliese 581 d, which is also potentially habitable, was discovered. (There are smaller planets known around a neutron star, named PSR B1257+12.) The discoverers estimate its radius to be 1.5 times that of the Earth.

Gliese 581 c and d are within the habitable zone of the host star, and are two of the most likely candidates for habitability of any extrasolar planets discovered so far.[13] Gliese 581 g, detected September 2010,[14] has a near-circular orbit in the middle of the star's habitable zone. However, the planet's existence is contested.[15]

Habitability[edit]

An artist's impression of a planet with two exomoons orbiting in the habitable zone of a red dwarf.

Planetary habitability of red dwarf systems is subject to some debate. In spite of their great numbers and long lifespans, there are several factors which may make life difficult on planets around a red dwarf. First, planets in the habitable zone of a red dwarf would be so close to the parent star that they would likely be tidally locked. This would mean that one side would be in perpetual daylight and the other in eternal night. This could create enormous temperature variations from one side of the planet to the other. Such conditions would appear to make it difficult for forms of life similar to those on Earth to evolve. And it appears there is a great problem with the atmosphere of such tidally locked planets: the perpetual night zone would be cold enough to freeze the main gases of their atmospheres, leaving the daylight zone nude and dry. On the other hand, recent theories propose that either a thick atmosphere or planetary ocean could potentially circulate heat around such a planet. Alternatively, a moon in orbit around a gas giant planet may be habitable. It would circumvent the tidal lock problem by becoming tidally locked to its planet. This way there would be a day/night cycle as the moon orbited its primary, and there would be distribution of heat.

In addition, red dwarfs emit most of their radiation as infrared light, while on Earth plants use energy mostly in the visible spectrum. Red dwarfs emit almost no ultraviolet light, which would be a problem, should this kind of light be required for life to exist. Variability in stellar energy output may also have negative impacts on development of life. Red dwarfs are often covered by starspots, reducing stellar output by as much as 40% for months at a time. At other times, some red dwarfs, called flare stars, can emit gigantic flares, doubling their brightness in minutes. This variability may also make it difficult for life to develop and persist near a red dwarf. Gibor Basri of the University of California, Berkeley claims a planet orbiting close to a red dwarf could keep its atmosphere even if the star flares.[16]

Spectral standard stars[edit]

Gliese 623b is right of center

The spectral standards for M-type stars have changed slightly over the years, but settled down somewhat since the early 1990s. Part of this is due to the fact that even the nearest M dwarfs are fairly faint, and the study of mid- to late-M dwarfs has only taken off in the past few decades due to evolution of astronomical techniques, from photographic plates to charged-couple devices (CCDs) to infrared-sensitive arrays.

The revised Yerkes Atlas system (Johnson & Morgan 1953)[17] listed only 2 M-type spectral standard stars: HD 147379 (M0 V) and HD 95735/Lalande 21185 (M2 V). While HD 147379 was not considered a standard by expert classifiers in later compendia of standards, Lalande 21185 is still a primary standard for M2 V. Robert Garrison[18] does not list any "anchor" standards among the M dwarf stars, but Lalande 21185 has survived as a M2 V standard through many compendia.[17][19][20] The review on MK classification by Morgan & Keenan (1973) did not contain M dwarf standards. In the mid-1970s, M dwarf standard stars were published by Keenan & McNeil (1976)[21] and Boeshaar (1976),[22] but unfortunately there was little agreement among the standards. As later cooler stars were identified through the 1980s, it was clear that an overhaul of the M dwarf standards was needed. Building primarily upon the Boeshaar standards, a group at Steward Observatory (Kirkpatrick, Henry, & McCarthy 1991)[23] filled in the spectral sequence from K5 V to M9 V. It is these M type dwarf standard stars which have largely survived intact as the main standards to the modern day. There have been negligible changes in the M dwarf spectral sequence since 1991. Additional M dwarf standards were compiled by Henry et al. (2002),[24] and D. Kirkpatrick has recently reviewed the classification of M dwarf stars and standard stars in Gray & Corbally's 2009 monograph.[25] The M-dwarf primary spectral standards are: GJ 270 (M0 V), GJ 229A (M1 V), Lalande 21185 (M2 V), GJ 752A (M3 V), GJ 402 (M4 V), GJ 51 (M5 V), Wolf 359 (M6 V), Van Biesbroeck 8 (M7 V), VB 10 (M8 V), LHS 2924 (M9 V).

See also[edit]

References[edit]

  1. ^ "The Brightest Red Dwarf", by Ken Croswell (Accessed 6/7/08)
  2. ^ Exoplanets near red dwarfs suggest another Earth nearer, 6 february 2013, Jason Palmer, BBC, retrieved at 11 april 2013
  3. ^ Reiners, A.; Basri, G. (March 2009). "On the magnetic topology of partially and fully convective stars". Astronomy and Astrophysics 496 (3): 787–790. arXiv:0901.1659. Bibcode:2009A&A...496..787R. doi:10.1051/0004-6361:200811450. 
  4. ^ a b Richmond, Michael (November 10, 2004). "Late stages of evolution for low-mass stars". Rochester Institute of Technology. Retrieved 2007-09-19. 
  5. ^ Chabrier, G.; Baraffe, I.; Plez, B. (1996). "Mass-Luminosity Relationship and Lithium Depletion for Very Low Mass Stars". Astrophysical Journal Letters 459 (2): L91–L94. Bibcode:1996ApJ...459L..91C. doi:10.1086/309951. 
  6. ^ Padmanabhan, Thanu (2001). Theoretical Astrophysics. Cambridge University Press. pp. 96–99. ISBN 0-521-56241-4. 
  7. ^ Kaltenegger, Lisa; Traub, Wesley A. (June 2009). "Transits of Earth-like Planets". The Astrophysical Journal 698 (1): 519–527. arXiv:0903.3371. Bibcode:2009ApJ...698..519K. doi:10.1088/0004-637X/698/1/519. 
  8. ^ a b c Adams, Fred C.; Laughlin, Gregory; Graves, Genevieve J. M. "Red Dwarfs and the End of the Main Sequence". Gravitational Collapse: From Massive Stars to Planets. Revista Mexicana de Astronomía y Astrofísica. pp. 46–49. Bibcode:2004RMxAC..22...46A. 
  9. ^ Fred C. Adams and Gregory Laughlin (1996). "A Dying Universe: The Long Term Fate and Evolution of Astrophysical Objects". Reviews of Modern Physics 69 (2): 337–372. arXiv:astro-ph/9701131. Bibcode:1997RvMP...69..337A. doi:10.1103/RevModPhys.69.337. 
  10. ^ Koupelis, Theo (2007). In Quest of the Universe. Jones & Bartlett Publishers. ISBN 0-7637-4387-9. 
  11. ^ J. A. Johnson (2011). "The Stars that Host Planets". Sky & Telescope (April): 22–27. 
  12. ^ Billions of Rocky Planets in Habitable Zones Around Red Dwarfs European Southern Observatory March 28, 2012
  13. ^ Major Discovery: New Planet Could Harbor Water and Life By Ker Than (Staff Writer) 24 April 2007 SPACE.com
  14. ^ "Scientists find potentially habitable planet near Earth". Physorg.com. Retrieved 2013-03-26. 
  15. ^ Mikko Tuomi (2011). "Bayesian re-analysis of the radial velocities of Gliese 581. Evidence in favour of only four planetary companions". arXiv:1102.3314 [astro-ph.EP].
  16. ^ Scientific American, "Red Star Rising", Mark Alpert, 2005 November 7
  17. ^ a b 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
  18. ^ MK ANCHOR POINTS, Robert F. Garrison
  19. ^ 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.
  20. ^ A standard stellar spectral sequence in the red/near-infrared – Classes K5 to M9 Kirkpatrick, J. D.; Henry, Todd J.; McCarthy, Donald W., Jr., 1991, Astrophysical Journal Supplement Series, vol. 77, Nov. 1991, p. 417
  21. ^ An atlas of spectra of the cooler stars: Types G,K,M,S, and C. Part 1: Introduction and tables P.C. Keenan & R.C. McNeil, 1976, Columbus: Ohio State University Press
  22. ^ The spectral classification of M-dwarf stars Boeshaar, P.C, 1976, Ph.D. Thesis Ohio State Univ., Columbus.
  23. ^ A standard stellar spectral sequence in the red/near-infrared – Classes K5 to M9 Kirkpatrick, J. D.; Henry, Todd J.; McCarthy, Donald W., Jr., 1991, Astrophysical Journal Supplement Series, vol. 77, Nov. 1991, p. 417-440
  24. ^ The Solar Neighborhood. VI. New Southern Nearby Stars Identified by Optical Spectroscopy Henry, Todd J.; Walkowicz, Lucianne M.; Barto, Todd C.; Golimowski, David A., 2002, The Astronomical Journal, Volume 123, Issue 4, pp. 2002–2009
  25. ^ Stellar Spectral Classification Richard O. Gray and Christopher J. Corbally, 2009, Princeton University Press. ISBN 978-0-691-12511-4
Notes

External links[edit]