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Red dwarf

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(Redirected from M-type main sequence star)
This article is about the type of star. For the British comedy franchise, see Red Dwarf.
"M dwarf" redirects here. For substellar objects, see brown dwarf.
Proxima Centauri, the closest star to the Sun, at a distance of 4.2 ly (1.3 pc), is a red dwarf.

A red dwarf is the smallest kind of star on the main sequence. Red dwarfs are by far the most common type of fusing star in the Milky Way, at least in the neighborhood of the Sun. However, due to their low luminosity, individual red dwarfs cannot be easily observed. From Earth, not one star that fits the stricter definitions of a red dwarf is visible to the naked eye.[1] Proxima Centauri, the star nearest to the Sun, is a red dwarf, as are fifty of the sixty nearest stars. According to some estimates, red dwarfs make up three-quarters of the fusing stars in the Milky Way.[2]

The coolest red dwarfs near the Sun have a surface temperature of about 2,000 K and the smallest have radii about 9% that of the Sun, with masses about 7.5% that of the Sun. These red dwarfs have spectral types of L0 to L2. There is some overlap with the properties of brown dwarfs, since the most massive brown dwarfs at lower metallicity can be as hot as 3,600 K and have late M spectral types.

Definitions and usage of the term "red dwarf" vary on how inclusive they are on the hotter and more massive end. One definition is synonymous with stellar M dwarfs (M-type main sequence stars), yielding a maximum temperature of 3,900 K and 0.6 M☉. One includes all stellar M-type main-sequence and all K-type main-sequence stars (K dwarf), yielding a maximum temperature of 5,200 K and 0.8 M☉. Some definitions include any stellar M dwarf and part of the K dwarf classification. Other definitions are also in use. Many of the coolest, lowest mass M dwarfs are expected to be brown dwarfs, not true stars, and so those would be excluded from any definition of red dwarf.

Stellar models indicate that red dwarfs less than 0.35 M☉ are fully convective.[3] Hence, the helium produced by the thermonuclear fusion of hydrogen is constantly remixed throughout the star, avoiding helium buildup at the core, thereby prolonging the period of fusion. Low-mass red dwarfs therefore develop very slowly, maintaining a constant luminosity and spectral type for trillions of years, until their fuel is depleted. Because of the comparatively short age of the universe, no red dwarfs yet exist at advanced stages of evolution.

Definition

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The term "red dwarf" when used to refer to a star does not have a strict definition. One of the earliest uses of the term was in 1915, used simply to contrast "red" dwarf stars from hotter "blue" dwarf stars.[4] It became established use, although the definition remained vague.[5] In terms of which spectral types qualify as red dwarfs, different researchers picked different limits, for example K8–M5[6] or "later than K5".[7] Dwarf M star, abbreviated dM, was also used, but sometimes it also included stars of spectral type K.[8]

In modern usage, the definition of a red dwarf still varies. When explicitly defined, it typically includes late K- and early to mid-M-class stars,[9] but in many cases it is restricted just to M-class stars.[10][11] In some cases all K stars are included as red dwarfs,[12] and occasionally even earlier stars.[13]

The most recent surveys place the coolest true main-sequence stars into spectral types L2 or L3. At the same time, many objects cooler than about M6 or M7 are brown dwarfs, insufficiently massive to sustain hydrogen-1 fusion.[14] This gives a significant overlap in spectral types for red and brown dwarfs. Objects in that spectral range can be difficult to categorize.

Description and characteristics

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Red dwarfs are very-low-mass stars.[15] As a result, they have relatively low pressures, a low fusion rate, and hence, a low temperature. The energy generated is the product of nuclear fusion of hydrogen into helium by way of the proton–proton (PP) chain mechanism. Hence, these stars emit relatively little light, sometimes as little as 1⁄10,000 that of the Sun, although this would still imply a power output on the order of 1022 watts (10 trillion gigawatts or 10 ZW). Even the largest red dwarfs (for example HD 179930, HIP 12961 and Lacaille 8760) have only about 10% of the Sun's luminosity.[16] In general, red dwarfs less than 0.35 M☉ 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, a red dwarf will have a region around its core where convection does not occur.[17]

The predicted main-sequence lifetime of a red dwarf plotted against its mass relative to the Sun.[18]

Because low-mass 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 less than 0.8 M☉ 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 the Sun by the third or fourth power of the ratio of the solar mass to their masses; thus, a 0.1 M☉ red dwarf may continue burning for 10 trillion years.[15][19] 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 released by this size reduction is converted into heat, which is carried throughout the star by convection.[20]

Properties of typical M-type main-sequence stars[21][22][23]
Spectral
type[24] 		Mass (M☉) Radius (R☉) Luminosity (L☉) Effective
temperature
(K) 		Color
index
(B − V)
M0V 0.57 0.588 0.069 3,850 1.42
M1V 0.50 0.501 0.041 3,660 1.49
M2V 0.44 0.446 0.029 3,560 1.51
M3V 0.37 0.361 0.016 3,430 1.53
M4V 0.23 0.274 7.2x10−3 3,210 1.65
M5V 0.162 0.196 3.0x10−3 3,060 1.83
M6V 0.102 0.137 1.0x10−3 2,810 2.01
M7V 0.090 0.120 6.5x10−4 2,680 2.12
M8V 0.085 0.114 5.2x10−4 2,570 2.15
M9V 0.079 0.102 3.0x10−4 2,380 2.17

According to computer simulations, the minimum mass a red dwarf must have to eventually evolve into a red giant is 0.25 M☉; less massive objects, as they age, would increase their surface temperatures and luminosities becoming blue dwarfs and finally white dwarfs.[18]

The less massive the star, the longer this evolutionary process takes. A 0.16 M☉ red dwarf (approximately the mass of the nearby Barnard's Star) would stay on the main sequence for 2.5 trillion years, followed by five billion years as a blue dwarf, during which the star would have one third of the Sun's luminosity (L☉) and a surface temperature of 6,500–8,500 kelvins.[18]

The fact that red dwarfs and other low-mass stars still remain on the main sequence when 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 move off the main sequence. This provides a lower limit to the age of the Universe and also allows formation timescales to be placed upon the structures within the Milky Way, such as the Galactic halo and Galactic disk.

All observed red dwarfs contain "metals", which in astronomy are elements heavier than hydrogen and helium. The Big Bang model predicts that the first generation of stars should have only hydrogen, helium, and trace amounts of lithium, and hence would be of low metallicity. With their extreme lifespans, any red dwarfs that were a part of that first generation (population III stars) should still exist today. Low-metallicity red dwarfs, however, are rare. The accepted model for the chemical evolution of the universe anticipates such a scarcity of metal-poor dwarf stars because only giant stars are thought to have formed in the metal-poor environment of the early universe.[why?] As giant stars end their short lives in supernova explosions, they spew out the heavier elements needed to form smaller stars. Therefore, dwarfs became more common as the universe aged and became enriched in metals. While the basic scarcity of ancient metal-poor red dwarfs is expected, observations have detected even fewer than predicted. The sheer difficulty of detecting objects as dim as red dwarfs was thought to account for this discrepancy, but improved detection methods have only confirmed the discrepancy.[25]

The boundary between the least massive red dwarfs and the most massive brown dwarfs depends strongly on the metallicity. At solar metallicity the boundary occurs at about 0.07 M☉, while at zero metallicity the boundary is around 0.09 M☉. At solar metallicity, the least massive red dwarfs theoretically have temperatures around 1,700 K, while measurements of red dwarfs in the solar neighbourhood suggest the coolest stars have temperatures of about 2,075 K and spectral classes of about L2. Theory predicts that the coolest red dwarfs at zero metallicity would have temperatures of about 3,600 K. The least massive red dwarfs have radii of about 0.09 R☉, while both more massive red dwarfs and less massive brown dwarfs are larger.[14][26]

Spectral standard stars

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Gliese 623 is a pair of red dwarfs, with GJ 623a on the left and the fainter GJ 623b to the 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 red dwarfs are fairly faint, and their colors do not register well on photographic emulsions used in the early to mid 20th century. The study of mid- to late-M dwarfs has significantly advanced only in the past few decades, primarily due to development of new astrographic and spectroscopic techniques, dispensing with photographic plates and progressing to charged-couple devices (CCDs) and infrared-sensitive arrays.

The revised Yerkes Atlas system (Johnson & Morgan, 1953)[27] listed only two M type spectral standard stars: HD 147379 (M0V) and HD 95735/Lalande 21185 (M2V). While HD 147379 was not considered a standard by expert classifiers in later compendia of standards, Lalande 21185 is still a primary standard for M2V. Robert Garrison[28] does not list any "anchor" standards among the red dwarfs, but Lalande 21185 has survived as a M2V standard through many compendia.[27][29][30] The review on MK classification by Morgan & Keenan (1973) did not contain red dwarf standards.

In the mid-1970s, red dwarf standard stars were published by Keenan & McNeil (1976)[31] and Boeshaar (1976),[32] but there was little agreement among the standards. As later cooler stars were identified through the 1980s, it was clear that an overhaul of the red dwarf standards was needed. Building primarily upon the Boeshaar standards, a group at Steward Observatory (Kirkpatrick, Henry, & McCarthy, 1991)[30] filled in the spectral sequence from K5V to M9V. It is these M type dwarf standard stars which have largely survived as the main standards to the modern day. There have been negligible changes in the red dwarf spectral sequence since 1991. Additional red dwarf standards were compiled by Henry et al. (2002),[33] and D. Kirkpatrick has recently reviewed the classification of red dwarfs and standard stars in Gray & Corbally's 2009 monograph.[34] The M dwarf primary spectral standards are: GJ 270 (M0V), GJ 229A (M1V), Lalande 21185 (M2V), Gliese 581 (M3V), Gliese 402 (M4V), GJ 51 (M5V), Wolf 359 (M6V), van Biesbroeck 8 (M7V), VB 10 (M8V), LHS 2924 (M9V).

Planets

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Illustration depicting AU Mic, an M-type (spectral class M1Ve) red dwarf star less than 0.7% the age of the Sun. The dark areas represent huge sunspot-like regions.

Many red dwarfs are orbited by exoplanets, but large Jupiter-sized planets are comparatively rare. Doppler surveys of a wide variety of stars indicate about 1 in 6 stars with twice the mass of the Sun are orbited by one or more of Jupiter-sized planets, versus 1 in 16 for Sun-like stars and the frequency of close-in giant planets (Jupiter size or larger) orbiting red dwarfs is only 1 in 40.[35] On the other hand, microlensing surveys indicate that long-orbital-period Neptune-mass planets are found around one in three red dwarfs.[36] 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.[37] Computer simulations of the formation of planets around low-mass stars predict that Earth-sized planets are most abundant, but more than 90% of the simulated planets are at least 10% water by mass, suggesting that many Earth-sized planets orbiting red dwarf stars are covered in deep oceans.[38]

At least four and possibly up to six exoplanets were discovered orbiting within the Gliese 581 planetary system between 2005 and 2010. One planet has about the mass of Neptune, or 16 Earth masses (ME). It orbits just 6 million kilometres (0.040 AU) from its star, and is estimated to have a surface temperature of 150 °C (423 K; 302 °F), despite the dimness of its star. In 2006, an even smaller exoplanet (only 5.5 ME) was found orbiting the red dwarf OGLE-2005-BLG-390L; it lies 390 million kilometres (2.6 AU) from the star and its surface temperature is −220 °C (53.1 K; −364.0 °F).

In 2007, a new, potentially habitable exoplanet, Gliese 581c, was found, orbiting Gliese 581. The minimum mass estimated by its discoverers (a team led by Stephane Udry) is 5.36 ME. The discoverers estimate its radius to be 1.5 times that of Earth (R🜨). Since then Gliese 581d, which is also potentially habitable, was discovered.

Gliese 581c and d are within the habitable zone of the host star, and are two of the most likely candidates for habitability of any exoplanets discovered so far.[39] Gliese 581g, detected September 2010,[40] has a near-circular orbit in the middle of the star's habitable zone. However, the planet's existence is contested.[41]

On 23 February 2017 NASA announced the discovery of seven Earth-sized planets orbiting the red dwarf star TRAPPIST-1 approximately 39 light-years away in the constellation Aquarius. The planets were discovered through the transit method, meaning we have mass and radius information for all of them. TRAPPIST-1e, f, and g appear to be within the habitable zone and may have liquid water on the surface.[42]

Habitability

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Main article: Habitability of red dwarf systems
An artist's impression of a planet with two exomoons orbiting in the habitable zone of a red dwarf.

Modern evidence suggests that planets in red dwarf systems are extremely unlikely to be habitable. 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. For a nearly circular orbit, 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 bare and dry. On the other hand, though, a theory proposes that either a thick atmosphere or planetary ocean could potentially circulate heat around such a planet.[43]

Variability in stellar energy output may also have negative impacts on the development of life. Red dwarfs are often flare stars, which can emit gigantic flares, doubling their brightness in minutes. This variability makes it difficult for life to develop and persist near a red dwarf.[44] While it may be possible for a planet orbiting close to a red dwarf to keep its atmosphere even if the star flares, more-recent research suggests that these stars may be the source of constant high-energy flares and very large magnetic fields, diminishing the possibility of life as we know it.[45][46]

See also

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References

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  2. ^ Jason Palmer (6 February 2013). "Exoplanets near red dwarfs suggest another Earth nearer". BBC. Retrieved 2019-07-10.
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  4. ^ Lindemann, F. A. (1915). "The age of the Earth". The Observatory. 38: 299. Bibcode:1915Obs....38..299L.
  5. ^ Edgeworth, K. E. (1946). "Red Dwarf Stars". Nature. 157 (3989): 481. Bibcode:1946Natur.157..481E. doi:10.1038/157481d0. S2CID 4106298.
  6. ^ Dyer, Edward R. (1956). "An analysis of the space motions of red dwarf stars". Astronomical Journal. 61: 228. Bibcode:1956AJ.....61..228D. doi:10.1086/107332.
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  19. ^ Fred C. Adams & Gregory Laughlin (1997). "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. S2CID 12173790.
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  24. ^ Younger brown dwarfs may also exhibit spectra similar to late M-type stars.
  25. ^ Elisabeth Newton (Feb 15, 2012). "And now there's a problem with M dwarfs, too". Astrobites. Retrieved 2019-07-10.
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  30. ^ a b Kirkpatrick, J.D.; Henry, Todd J.; McCarthy, Donald W. (1991). "A standard stellar spectral sequence in the red / near-infrared - Classes K5 to M9". Astrophysical Journal Supplement Series. 77: 417. Bibcode:1991ApJS...77..417K. doi:10.1086/191611.
  31. ^ Keenan, Philip Childs; McNeil, Raymond C. (1976). An atlas of spectra of the cooler stars: Types G, K, M, S, and C. Part 1: Introduction and tables. Columbus, OH: Ohio State University Press. Bibcode:1976aasc.book.....K.
  32. ^ Boeshaar, P.C. (1976). The spectral classification of M dwarf stars (Ph.D. thesis). Columbus, OH: Ohio State University. Bibcode:1976PhDT........14B.
  33. ^ Henry, Todd J .; Walkowicz, Lucianne M.; Barto, Todd C.; Golimowski, David A. (2002). "The Solar neighborhood. VI. New southern nearby stars identified by optical spectroscopy". The Astronomical Journal. 123 (4): 2002. arXiv:astro-ph/0112496. Bibcode:2002AJ....123.2002H. doi:10.1086/339315. S2CID 17735847.
  34. ^ Gray, Richard O.; Corbally, Christopher (2009). Stellar Spectral Classification. Princeton University Press. Bibcode:2009ssc..book.....G.
  35. ^ Mawet, Dimitri; Jovanovic, Nemanja; Delorme, Jacques-Robert; et al. (2018-07-10). "Keck Planet Imager and Characterizer (KPIC): status update" (PDF). In Schmidt, Dirk; Schreiber, Laura; Close, Laird M. (eds.). Adaptive Optics Systems VI. SPIE. p. 6. doi:10.1117/12.2314037. ISBN 9781510619593. Close separations (< 1 AU) have been extensively probed by Doppler and transit surveys with the following results: the frequency of close-in giant planets (1−10 MJup) is only 2.5 ± 0.9%, consistent with core accretion plus migration models.
  36. ^ Johnson, J.A. (April 2011). "The stars that host planets". Sky & Telescope. pp. 22–27.
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  41. ^ Tuomi, Mikko (2011). "Bayesian re-analysis of the radial velocities of Gliese 581. Evidence in favour of only four planetary companions". Astronomy & Astrophysics. 528: L5. arXiv:1102.3314. Bibcode:2011A&A...528L...5T. doi:10.1051/0004-6361/201015995. S2CID 11439465.
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  46. ^ George Dvorsky (2015-11-19). "This Stormy Star Means Alien Life May Be Rarer Than We Thought". Gizmodo. Retrieved 2019-07-10.

Sources

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