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51 Pegasi is a yellow-orange star
like our Sun, Sol. (See a Digitized
Sky Survey image of 51 Pegasi
from the Nearby Stars Database.)
51 Pegasi is located about 50.1 light-years from Sol. It lies near the center (22:57:28+20:46:7.8, ICRS 2000.0) of Constellation Pegasus, the Winged Horse -- northwest of Markab (Alpha Pegasi) and southwest of Scheat (Beta Pegasi). In 1995, astronomers announced the discovery of a Jupiter-class planet around this Sun-like star (Mayor and Queloz, 1995; and 51 Pegasi at the Observatoire de Genève -- details below). (See an animation of the planetary and potentially habitable zone orbits of this system, with a table of basic orbital and physical characteristics.)
© James B. Kaler, UIUC -- more information
(Photo from Stars, Planet Project, and 51 Pegasi; used with permission)
As 51 Pegasi has become one of the top 100 target stars for NASA's planned Terrestrial Planet Finder (TPF), images of this star and its position relative to the Milky Way in Earth's night sky are now available from the TPF-C team. On February 19, 2006, Margaret Turnbull named 51 Pegasi as a Sun-like star that is old enough to qualify as a top-five candidate for those listening for radio signals from intelligent civilizations, such as the SETI Institute.
Astronomers have identified 51
Pegasi as a prime target for the
Terrestrial Planet Finder (TPF),
now planned for launch between
2014 and 2020.
51 Pegasi is a yellow-orange main sequence dwarf star of spectral and luminosity type G4-5 Va, but it had been previously classified as G2-2.5 and sometimes as a subgiant (IV). The star has about 1.06 times the mass of Sol (51 Peg at exoplanets.org), 1.15 to 1.4 times its diameter (Henry et al, 2000; and Guillot et al, 1996), and 1.30 times its visual luminosity (51 Pegasi at the Observatoire de Genève). Relatively bright and large for its spectral type and mass, it appears to be running low on core hydrogen and may be as old as 8.5 billion years old or more (Henry et al, 1997), but one analysis of isochrones suggests that the star could be a billion years younger -- at 7.5 billion years old (Guinan et al, 1999). 51 Pegasi is 1.6 times more enriched than Sol with elements heavier than hydrogen ("metallicity"), based on its abundance of iron (51 Peg at exoplanets.org). It is a New Suspected Variable (NSV) 14374. Useful catalogue numbers and designations for the star include: 51 Peg, HR 8729, Gl 882, Hip 113357, HD 217014, BD+19 5036, SAO 90896, and LTT 16750.
© Tomislav Stimac -- larger image
Artwork from Planets at Digital Eye
(used with permission).
A "naked-eye" view of 51 Pegasi and its
close planetary companion "b" (800,000 km
from the surface of b and 7.7 million km
from the star), as simulated by Stimac (more).
Whatmough -- larger image
(Artwork from Extrasolar Visions, used with permission)
Planet b could be an extremely hot, rocky
superplanet, as imagined by Whatmough.
In 1995, astronomers (Michel Mayor and Didier Queloz) announced the discovery of a Jupiter-class planet around 51 Pegasi using radial-velocity methods (Mayor and Queloz, 1995; and 51 Pegasi at the Observatoire de Genève). Planet "b" has at least 46 percent of Jupiter's mass. It moves around 51 Pegasi at an average distance of only 0.05 AUs (a semi-major axis well within Mercury's orbital distance) in a highly circular orbit (e=0.03) that takes only 4.2 days to complete. Its orbit may be inclined by less than 85° from the perspective of an observer on Earth (Henry et al, 1997). Assuming a Jupiter-like composition, its radius may be about 1.2 times that of Jupiter, enlarged relative to Jupiter because of greater absorbed stellar radiation in its inner ("torch") orbit. However, the planet may be too hot to hold onto a thick hydrogen atmosphere (discussion).
© Christoph Kulmann -- larger image
Artwork from Exoplaneten.de
(used with permission).
The surface of 51 Pegasi "b" as an
extremely hot, supermassive rocky
planet with a dense atmosphere, as
imagined by Kulmann (more).
Recently, astronomers at the University of Texas at Arlington performed refined calculations to determine that the habitable zone around 51 Pegasi, where an inner rocky planet (with suitable mass and atmospheric gas composition and density) can have liquid water on its surface, lies between 1.20 and 2.0 AUs of the star. Unfortunately, the development of an Earth-like planet in this zone could have been disrupted since it would likely be expelled by the inward migration of planet b, as hypothesized by some planetary astronomers. If a small, rocky planet could have developed without the interference of planet b, however, then stable orbits appear to be possible over the entire habitable zone (news release; and Noble et al, 2002, in pdf).
Noble, Musielak, and Cuntz (2002,
University of Texas at Arlington
Larger chart with terrestrial planet
in an inner orbit, located in the first
tenth of the habitable zone distance.
Stable orbits for a Earth-type, rocky
inner planet over the entire habitable
zone (1.2 to 2.0 AUs), if such a planet
could develop without being expelled
by the hypothesized inward migration
of planet b (news release).
A terrestrial planet orbiting 51 Pegasi at around the center of the calculated habitable zone would have an average orbital distance of about 1.6 AU, just beyond the orbit of Mars (towards the Main Asteroid Belt) in the Solar System. It would complete this orbit within about 2.0 years. (See an animation of the planetary and potentially habitable zone orbits of this system, with a table of basic orbital and physical characteristics.) Astronomers are hoping to use NASA's Terrestrial Planet Finder (TPF) and the ESA's Darwin planned groups of observatories to search for a rocky inner planet in the so-called "habitable zone" (HZ) around 51 Pegasi. As currently planned, the TPF will include two complementary observatory groups: a visible-light coronagraph to launch around 2014; and a "formation-flying" infrared interferometer to launch before 2020, while Darwin will launch a flotilla of three mid-infrared telescopes and a fourth communications hub beginning in 2015.
The following table includes all star systems known to be located within 10 light-years (ly), plus more bright stars within 10 to 20 ly, of 51 Pegasi.
|Star System||Spectra &|
|Steph 2065||M0 V||3.0|
|Xi Pegasus2?||F6-7 V-III |
|G 127-50||M V||3.9|
|L 1295-9||M4 V||9.0|
|AC+31 70565||M3.5 Ve||9.5|
|LTT 16719||M3.5 Ve||10.0|
|* plus bright stars *||. . .|
|BD+18 5200||G0 V||12|
|Iota Pegasi 2||F5 V |
|85 Pegasi 3||G5 Vb |
|Iota Piscium 2?||F7 V |
|Hip 109119||A2 V ||19|
Try Professor Jim Kaler's Stars site for other information about 51 Pegasi at the University of Illinois' Department of Astronomy. John Whatmough also has illustrated web pages on this system in Extrasolar Visions. For another illustrated discussion, see Christoph Kulmann's web page on 51 Pegasi.
Up-to-date technical summaries on this star can be found at: Jean Schneiders's Extrasolar Planets Encyclopaedia; the Astronomiches Rechen-Institut at Heidelberg's ARICNS, the Nearby Stars Database, and the Research Consortium on Nearby Stars (RECONS). Additional information may be available at Roger Wilcox's Internet Stellar Database.
The "Winged Horse" is one of the larger constellations of the Northern Hemisphere. For more information about the stars and objects in this constellation and an illustration, go to Christine Kronberg's Pegasus. For an illustration, see David Haworth's Pegasus.
For more information about stars including spectral and luminosity class codes, go to ChView's webpage on The Stars of the Milky Way.
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