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(Redirected from Red dwarf star)
:''This article is about the type of star known as a red dwarf. For the television programme, see ''Red Dwarf''.''
According to the Hertzsprung-Russell diagram, a 'red dwarf star' is a small and relatively cool star, of the main sequence, either late K or M spectral type. They constitute the vast majority of stars and have a mass of less than one-half that of the Sun (down to about 0.075 solar masses, which are brown dwarfs) and a surface temperature of less than 3,500 K.
Red dwarfs fuse hydrogen to helium via the proton-proton (PP) chain. Due to the low temperatures in the core, fusion proceeds slowly.
Consequently they emit little light, sometimes as little as 1/10,000th that of the sun.
In general red dwarfs transport energy from the core to the surface via convection. As red dwarfs are fully convective, they can burn a larger proportion of their hydrogen before leaving the main sequence than larger stars, such as the Sun.
Thus red dwarfs have an enormous estimated lifespan; from tens of billions up to trillions of years depending upon mass; the lower the mass, the longer the lifespan.
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 one to date star clusters 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 2007 is the absence of metals in red dwarf stars (in astronomy a metal is any element other than hydrogen or helium). The Big Bang model predicts the first generation of stars should have only hydrogen, helium, and lithium. If such stars included red dwarfs, they should still be observable today, but as yet none have been identified. One explanation is that without heavy elements, low mass stars cannot form. Alternatively as they are dim and could be few in number, we simply may not have observed them yet.
Red dwarfs are the most common star type in the Galaxy, at least in the neighborhood of the Sun. 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. However, due to their low luminosity, individual red dwarfs cannot easily be observed over the vast intergalactic distances that luminous stars can.
Extrasolar planets were discovered orbiting red dwarfs in 2005, one as small as the size of Neptune, or seventeen 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 how dim the star is. In 2006, an even smaller extrasolar planet (only 5.5 times the mass of Earth) was found orbiting a red dwarf; it lies 390 million km (2.6 AU) from the star and its surface temperature is −220 °C (56 K).
In 2007, a potentially habitable extrasolar planet, Gliese 581 c, was found, orbiting the red dwarf star Gliese 581. If the mass estimated by its discoverers (a team led by Stephane Udry), namely 5.03 times that of the Earth, is correct, it is the smallest extrasolar planet revolving around a normal star discovered to date. (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.
This planet is within the habitable zone of Gliese 581, and is the most likely candidate for habitability of any extrasolar planet discovered so far.[1]
Planetary habitability of red dwarf star 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 star. 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 life (as we know it) to evolve. On the other hand, recent theories propose that either a thick atmosphere or planetary ocean could potentially circulate heat around the planet. Another potential problem is that red dwarfs emit most of their radiation as infrared light, while on Earth plants use energy mostly in the visible spectrum. But, perhaps the most serious problem may be stellar variability. Red dwarfs are often covered in 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 as we know it to survive near a red dwarf star.
★ Cataclysmic variable star
★ Hertzsprung-Russell diagram
★ Red giant
★ Yerkes luminosity classification
★ Stellar evolution
★ White dwarf
★ Brown dwarf
★ Flare Star
★ Nemesis (star)
1. http://www.space.com/scienceastronomy/070424_hab_exoplanet.html
★ An expanded set of brown dwarf and very low mass star models, A. Burrows, W. B. Hubbard, D. Saumon, J. I. Lunine, , , Astrophysical Journal, 1993
★ VLT Interferometer Measures the Size of Proxima Centauri and Other Nearby Stars
★ Neptune-Size Planet Orbiting Common Star Hints at Many More
★ Variable stars
★ Stellar Flares - D. Montes, UCM.
★ Red Dwarfs
★ Red Star Rising : Small, cool stars may be hot spots for life - ''Scientific American'' (November 2005)
:''This article is about the type of star known as a red dwarf. For the television programme, see ''Red Dwarf''.''
An artist's impression of a planet in orbit around a red dwarf
According to the Hertzsprung-Russell diagram, a 'red dwarf star' is a small and relatively cool star, of the main sequence, either late K or M spectral type. They constitute the vast majority of stars and have a mass of less than one-half that of the Sun (down to about 0.075 solar masses, which are brown dwarfs) and a surface temperature of less than 3,500 K.
| Contents |
| Description and characteristics |
| Planets |
| Habitability |
| See also |
| References |
| External links |
Description and characteristics
Red dwarfs fuse hydrogen to helium via the proton-proton (PP) chain. Due to the low temperatures in the core, fusion proceeds slowly.
Consequently they emit little light, sometimes as little as 1/10,000th that of the sun.
In general red dwarfs transport energy from the core to the surface via convection. As red dwarfs are fully convective, they can burn a larger proportion of their hydrogen before leaving the main sequence than larger stars, such as the Sun.
Thus red dwarfs have an enormous estimated lifespan; from tens of billions up to trillions of years depending upon mass; the lower the mass, the longer the lifespan.
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 one to date star clusters 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 2007 is the absence of metals in red dwarf stars (in astronomy a metal is any element other than hydrogen or helium). The Big Bang model predicts the first generation of stars should have only hydrogen, helium, and lithium. If such stars included red dwarfs, they should still be observable today, but as yet none have been identified. One explanation is that without heavy elements, low mass stars cannot form. Alternatively as they are dim and could be few in number, we simply may not have observed them yet.
Red dwarfs are the most common star type in the Galaxy, at least in the neighborhood of the Sun. 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. However, due to their low luminosity, individual red dwarfs cannot easily be observed over the vast intergalactic distances that luminous stars can.
Planets
Extrasolar planets were discovered orbiting red dwarfs in 2005, one as small as the size of Neptune, or seventeen 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 how dim the star is. In 2006, an even smaller extrasolar planet (only 5.5 times the mass of Earth) was found orbiting a red dwarf; it lies 390 million km (2.6 AU) from the star and its surface temperature is −220 °C (56 K).
In 2007, a potentially habitable extrasolar planet, Gliese 581 c, was found, orbiting the red dwarf star Gliese 581. If the mass estimated by its discoverers (a team led by Stephane Udry), namely 5.03 times that of the Earth, is correct, it is the smallest extrasolar planet revolving around a normal star discovered to date. (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.
This planet is within the habitable zone of Gliese 581, and is the most likely candidate for habitability of any extrasolar planet discovered so far.[1]
Habitability
Planetary habitability of red dwarf star 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 star. 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 life (as we know it) to evolve. On the other hand, recent theories propose that either a thick atmosphere or planetary ocean could potentially circulate heat around the planet. Another potential problem is that red dwarfs emit most of their radiation as infrared light, while on Earth plants use energy mostly in the visible spectrum. But, perhaps the most serious problem may be stellar variability. Red dwarfs are often covered in 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 as we know it to survive near a red dwarf star.
See also
★ Cataclysmic variable star
★ Hertzsprung-Russell diagram
★ Red giant
★ Yerkes luminosity classification
★ Stellar evolution
★ White dwarf
★ Brown dwarf
★ Flare Star
★ Nemesis (star)
References
1. http://www.space.com/scienceastronomy/070424_hab_exoplanet.html
★ An expanded set of brown dwarf and very low mass star models, A. Burrows, W. B. Hubbard, D. Saumon, J. I. Lunine, , , Astrophysical Journal, 1993
★ VLT Interferometer Measures the Size of Proxima Centauri and Other Nearby Stars
★ Neptune-Size Planet Orbiting Common Star Hints at Many More
External links
★ Variable stars
★ Stellar Flares - D. Montes, UCM.
★ Red Dwarfs
★ Red Star Rising : Small, cool stars may be hot spots for life - ''Scientific American'' (November 2005)
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