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Coordinates: Sky map 15h 19m 26s, −07° 43′ 20″
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The parameters listed below come from an orbital fit in which eccentricities were fixed at 0. Allowing eccentricities to vary did not significantly improve the fit.<ref>pp. 15, 24, Vogt 2010.</ref>
The parameters listed below come from an orbital fit in which eccentricities were fixed at 0. Allowing eccentricities to vary did not significantly improve the fit.<ref>pp. 15, 24, Vogt 2010.</ref>


According to a presentation by F. Pepe at IAU Symposium 276, planet g was not detected in a new analysis of data taken by the HARPS spectrograph, and both planets f and g are listed as unconfirmed at the Extrasolar Planets Encyclopaedia.<ref>{{cite web|url=http://exoplanet.eu/star.php?st=Gl+581|title=Notes for star Gl 581|work=The Extrasolar Planets Encyclopaedia|accessdate=2010-10-11}}</ref>
According to a presentation by F. Pepe at IAU Symposium 276, planet g was not detected in a new analysis of data taken by the HARPS spectrograph,<ref name="unconfirmed">{{cite news| url=http://www.sciencenews.org/view/generic/id/64308/title/Existence_of_habitable_exoplanet_questioned | title= Existence of habitable exoplanet questioned |auctor= Ron Cowen| date=October 13 2010| work=Science News|accessdate=2010-10-14}}</ref> and both planets f and g are listed as unconfirmed at the Extrasolar Planets Encyclopaedia.<ref>{{cite web|url=http://exoplanet.eu/star.php?st=Gl+581|title=Notes for star Gl 581|work=The Extrasolar Planets Encyclopaedia|accessdate=2010-10-11}}</ref>


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{{PlanetboxOrbit begin

Revision as of 16:59, 14 October 2010

Gliese 581
File:Gliese 581.jpg
The star Gliese 581.
Digital Sky Survey photo.
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Libra
Right ascension 15h 19m 26.8250s[1]
Declination −07° 43′ 20.209″[1]
Apparent magnitude (V) 10.56 to 10.58a
Characteristics
Spectral type M3V[2]
B−V color index 1.61[1]
Variable type BYb
Astrometry
Radial velocity (Rv)−9.5 ± 0.5[1] km/s
Proper motion (μ) RA: −1233.51[3] mas/yr
Dec.: −94.52[3] mas/yr
Parallax (π)160.91 ± 2.62 mas[3]
Distance20.3 ± 0.3 ly
(6.2 ± 0.1 pc)
Absolute magnitude (MV)11.6[4]
Details
Mass0.31[5] M☉
Radius0.29[2] R☉
Luminosity (bolometric)0.013[2] L☉
Surface gravity (log g)4.92±0.10[6] cgs
Temperature3,480 ± 48[6] K
Metallicity[M/H] = −0.33 ± 0.12[6]
Age7 to 11[5][7] Gyr
Other designations
HO Librae, HO Lib, BD−07°4003, GJ 581, HIP 74995, LFT 1195, LHS 394, LPM 564, LTT 6112, NLTT 39886, TYC 5594-1093-1, Wolf 562.[1][8]
Database references
SIMBADdata

Gliese 581 (Template:Pron-en) is a red dwarf star with spectral type M3V, located 20.3 light years away from Earth in the constellation Libra. Its estimated mass is about a third of that of the Sun, and it is the 87th[9] closest known star system to the Sun. Observations suggest that the star has at least six planets: Gliese 581 e, b, c, g, d and f. Significantly, planet g is thought to be close to the middle of the star's habitable zone.[10][11]

The star system first gained attention after Gliese 581 c, the first low mass extrasolar planet found to be near its star's habitable zone, was discovered in April 2007. It has since been shown that under known terrestrial planet climate models, Gliese 581 c is likely to have a runaway greenhouse effect, and hence is probably too hot to be habitable, analogous to Venus. A subsequently discovered planet Gliese 581 d, may be just inside or just outside the outer boundary of the habitable zone (depending in part on the greenhouse properties of its atmosphere), analogous to Mars.[11] The discovery of exoplanet Gliese 581 e,[12] at that time the closest-known in mass to Earth, was announced in April 2009. Excitement spiked again in September 2010 with the discovery of Gliese 581 g, orbiting between c and d, believed to be the planet with the greatest likelihood of having conditions suitable for liquid water at its surface found to date.[13]

Star

The name Gliese 581 refers to the catalog number from the 1957 survey Gliese Catalogue of Nearby Stars of 965 stars located within 20 parsecs of the Earth. Other names of this star include BD-07° 4003 (BD catalogue, first known publication) and HO Librae (variable star designation). It does not have an individual name such as Sirius or Procyon.[1][8] The star is a red dwarf with spectral type M3V, located 20.3 light-years away from Earth. It is located about two degrees north of Beta Librae, the brightest star in the constellation Libra. Its mass is estimated to be approximately a third that of the Sun, and it is the 87th closest known star system to the Sun.[9]

Size of the Sun (left) and Gliese 581 (right).

An M-class dwarf star such as Gliese 581 has a much lower mass than the Sun, causing the core region of the star to fuse hydrogen at a significantly lower rate. From the apparent magnitude and distance, we can estimate an effective temperature of 3200 kelvins and a visual luminosity of 0.2% of that of the Sun.[14] However, a red dwarf such as Gliese 581 radiates primarily in the near infrared, with peak emission at a wavelength of roughly 830 nanometres (estimated using Wien's displacement law, which assumes the star radiates as a black body), so such an estimate will underestimate the star's total luminosity. (For comparison, the peak emission of the Sun is roughly 530 nanometres, in the middle of the visible part of the spectrum). When radiation over the entire spectrum is taken into account (not just the part that humans are able to see), something known as the bolometric correction, this star has a bolometric luminosity 1.3% of the Sun's total luminosity.[2][14] A planet would need to be situated much closer to this star in order to receive a comparable amount of energy as the Earth. The region of space around a star where a planet would receive roughly the same energy as the Earth is sometimes termed the "Goldilocks Zone", or, more prosaically, the habitable zone. The extent of such a zone is not fixed and is highly specific for each planetary system.[15]

Gliese 581 is classified as a variable star of the BY Draconis type, and has been given the variable star designation HO Librae. This is a star that exhibits variability because of the presence of star spots combined with the rotation of the star. However, the measured variability is close to the margin of error, and, if real, is most likely a long term variability. Gliese 581 appears too massive to be a flare star,[verification needed] which is a type of star that exhibits brief but intense outbursts of radiation that would make life less likely to survive.[16] Gliese 581 does emit X-rays.[17]

Planetary system

At least six planets are believed to be orbiting Gliese 581. Gliese 581 b, approximately Neptune-sized, was discovered in August 2005 and was the fifth planet to be discovered around a red dwarf star. This inner planet is at least 16 times as massive as Earth (similar to Neptune's mass) and completes a full orbit of Gliese 581 in only 5.4 days.[2]

The habitable zone of Gliese 581 compared with our Solar System's habitable zone.

Another planet, Gliese 581 c, was discovered in April 2007.[14] In their 2007 paper, Udry et al. assumed that if Gliese 581 c had a Earth-type composition, it would have a radius of 1.5R⊕, which would have made it at the time "the most Earth-like of all known exoplanets".[14]

A direct measurement of the radius cannot be taken because, viewed from Earth, the planet does not transit its sun. With a minimum mass of roughly five times Earth—or one third that of Neptune—Gliese 581 c orbits just inside of the habitable zone of its parent star.[18] The mean blackbody surface temperature has been estimated to lie between −3 °C (for a Venus-like albedo) and 40 °C (for an Earth-like albedo),[14] however, the temperatures could be much higher (about 500 degrees Celsius) due to a runaway greenhouse effect akin to that of Venus.[19] Some astronomers believe the system may have undergone planetary migration and Gliese 581 c may have formed beyond the frost line, with a composition similar to icy bodies like Ganymede. Gliese 581 c completes a full orbit in just under 13 days.[14]

Observations of the star also revealed a third planet, Gliese 581 d, with a mass of roughly 7 Earths, or half a Uranus, and an orbit of 66.8 Earth days.[14][20][21] It orbits just within the outer limit of the habitable zone of its star, which makes it a potential candidate for being able to support life.[12][19] (A reanalysis of the radial velocity data has reduced the minimum possible mass of this planet from 7.1 M⊕ to 5.6 M⊕.)[22]

4-body solution (2009)

2009 solution with elliptical orbits for c and d

Discovery of a fourth planet, Gliese 581 e, was announced on 21 April 2009. This planet, at an estimated minimum mass of 1.9 Earths, is currently the lowest mass exoplanet identified around a "normal star" (i.e. excluding pulsars). It takes 3.15 days to orbit Gliese 581.[12][21]

Dynamical simulations of the Gliese 581 system assuming that the orbits of planets b to d are coplanar show that the system becomes unstable if its component masses are more than 1.6 – 2 times the minimum mass. The upper limits on the masses of the planets are found to be 3.1, 30.4, 10.4 and 13.8 Earth masses for planets e, b, c and d respectively.[12]

The Gliese 581 planetary system[12]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
e 1.94 – 3.1 M🜨 0.03 3.14942 ± 0.00045 0 — —
b 15.65 – 30.4 M🜨 0.04 5.36874 ± 0.00019 0 — —
c 5.36 – 10.4 M🜨 0.07 12.9292 ± 0.0047 0.17 ± 0.07 — —
d 7.09 – 13.8 M🜨 0.22 66.80 ± 0.14 0.38 ± 0.09 — —

6-body solution (2010)

2010 solution, with circular orbits (outermost f excluded)
A National Science Foundation graphic comparing to our solar system, with f just outside the orbit of Venus

On 29 September 2010, astronomers at Keck Observatory announced the discovery of Gliese 581 f and Gliese 581 g, both in nearly circular orbits. The detection was based on analysis of a combination of data sets from the HIRES and HARPS instruments. Nicknamed Zarmina by one of its discoverers,[23] Gliese 581 g has a mass of 3 to 4 Earth-masses, with an orbital period of 37 days, and is at a distance from Gliese 581 that is well within the star's habitable zone. The planet is predicted to be tidally locked, with one side of the planet always facing the star.[11][24]

The approximate ratios of periods of adjacent orbits are (proceeding outward): 3:5, 2:5, 1:3, 1:2, 2:13.

The parameters listed below come from an orbital fit in which eccentricities were fixed at 0. Allowing eccentricities to vary did not significantly improve the fit.[25]

According to a presentation by F. Pepe at IAU Symposium 276, planet g was not detected in a new analysis of data taken by the HARPS spectrograph,[26] and both planets f and g are listed as unconfirmed at the Extrasolar Planets Encyclopaedia.[27]

The Gliese 581 planetary system[11]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
e ≥1.7 M🜨 0.0284533 ± 0.0000023 3.14867 ± 0.00039 0 — —
b ≥15.6 M🜨 0.0406163 ± 0.0000013 5.36841 ± 0.00026 0 — —
c ≥5.6 M🜨 0.072993 ± 0.000022 12.9191 ± 0.0058 0 — —
g (unconfirmed) ≥3.1 M🜨 0.14601 ± 0.00014 36.562 ± 0.052 0 — —
d ≥5.6 M🜨 0.21847 ± 0.00028 66.87 ± 0.13 0 — —
f (unconfirmed) ≥7.0 M🜨 0.758 ± 0.015 433 ± 13 0 — —

Radio signal sent from Earth

A Message From Earth (AMFE) is a high-powered digital radio signal that was sent on 9 October 2008 towards Gliese 581 c. The signal is a digital time capsule containing 501 messages that were selected through a competition on the social networking site, Bebo. The message was sent using the RT-70 radar telescope of Ukraine's National Space Agency. The signal will reach Gliese 581 in early 2029.

See also

Notes

  • Note a: Gl 581 is classified as a BY Draconis variable in the General Catalogue of Variable Stars.[28] This catalog gives a maximum magnitude of 10.56 and minimum of magnitude 10.58 for a relatively low 20 mmag (0.020 magnitudes) variability.[29] For full data see data description and "The combined table of GCVS Vols I-III and NL 67-78 with improved coordinates, General Catalogue of Variable Stars". Sternberg Astronomical Institute. Retrieved 27 April 2009.
  • Note b: In 1994 Edward Weis concluded that Gl 581, like half the 43 dwarf M stars he studied over a multi-year period, showed long term variability (and page 1137, Fig 1 shows Gl 581 had magnitude 10.58 in 1982 and between 10.57 and 10.56 from 1985 to 1990).[30] Bonfils noted in 2005 that "Gl 581 has been classified as a variable star (HO Lib), but its variability (Weis 1994) is only marginally significant. If real it would be on a time scale of several years, with short term variability being at most ∼0.006 mag."[31] Measurements by MOST showed short term variability of about 5 mmag (half a percent) over a period of a few weeks.[32]

References

  1. ^ a b c d e f GJ 581 , SIMBAD. Retrieved 2008-08-21.
  2. ^ a b c d e Bonfils, X. (2005). "The HARPS search for southern extra-solar planets VI: A Neptune-mass planet around the nearby M dwarf Gl 581". Astronomy and Astrophysics Letters. 443: L15–L18. Bibcode:2005A&A...443L..15B. doi:10.1051/0004-6361:200500193. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  3. ^ a b c van Leeuwen, F. (2007). "HIP 74995". Hipparcos, the New Reduction. Centre de données astronomiques de Strasbourg. Retrieved 16 August 2008.
  4. ^ From apparent magnitude and parallax.
  5. ^ a b "Star: Gl 581". Extrasolar Planets Encyclopaedia. Retrieved 27 April 2009. Mass 0.31 Msun, Age 8+3
    −1     Gyr
  6. ^ a b c Bean, J. L; Benedict, G. F.; Endl, M. (2006). "Metallicities of M Dwarf Planet Hosts from Spectral Synthesis". Astrophysical Journal Letters. 653 (1): L65–L68. Bibcode:2006ApJ...653L..65B. doi:10.1086/510527.
  7. ^ Selsis 3.4 page 1382 "lower limit of the age that, considering the associated uncertainties, could be around 7 Gyr", "preliminary estimate", "should not be above 10-11 Gyr"
  8. ^ a b "Entry 5594-1093-1". The Hipparcos and Tycho Catalogues. Centre de données astronomiques de Strasbourg. ID I/239.
  9. ^ a b "The One Hundred Nearest Star Systems". Research Consortium on Nearby Stars, Georgia State University. 1 January 2009. Retrieved 4 June 2010.
  10. ^ "Newly Discovered Planet May Be First Truly Habitable Exoplanet". ScienceDaily. 29 September 2010. Retrieved 1 October 2010.
  11. ^ a b c d Vogt, S. S. (2010). "The Lick-Carnegie Exoplanet Survey: A 3.1 M_Earth Planet in the Habitable Zone of the Nearby M3V Star Gliese 581". arXiv:1009.5733 [astro-ph.EP]. {{cite arXiv}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  12. ^ a b c d e Mayor, M. (2009). "The HARPS search for southern extra-solar planets XVIII: An Earth-mass planet in the GJ 581 planetary system" (PDF). Astronomy and Astrophysics. 507: 487. Bibcode:2009A&A...507..487M. doi:10.1051/0004-6361/200912172. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  13. ^ "US scientists find potentially habitable planet near Earth". Yahoo News. 29 September 2010. Retrieved 30 September 2010.
  14. ^ a b c d e f g Udry, S (2007). "The HARPS search for southern extra-solar planets XI: Super-Earths (5 and 8 M⊕) in a 3-planet system" (PDF). Astronomy and Astrophysics Letters. 469 (3): L43–L47. doi:10.1051/0004-6361:20077612. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  15. ^ Selsis, F. (2007). "Habitable planets around the star Gl 581?". Astronomy and Astrophysics. 476 (3): 1373–1387. Bibcode:2007A&A...476.1373. doi:10.1051/0004-6361:20078091. {{cite journal}}: Check |bibcode= length (help); Unknown parameter |coauthors= ignored (|author= suggested) (help)
  16. ^ Minard, A. (21 April 2009). "Nearly Earth-sized Planet, Possible Watery World Spotted Near Another Star". Universe Today. Retrieved 30 September 2010.
  17. ^ Schmitt, J. H. M. M; Fleming, T. A; Giampapa, M. S. (1995). "The X-Ray View of the Low-Mass Stars in the Solar Neighborhood". Astrophysical Journal. 450 (9): 392–400. Bibcode:1995ApJ...450..392S. doi:10.1086/176149.
  18. ^ von Bloh, W. (2008). "Habitability of Super-Earths: Gliese 581c & 581d". Proceedings of the International Astronomical Union. 3 (S249): 503–506. doi:10.1017/S1743921308017031. arXiv:0712.3219. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  19. ^ a b von Bloh, W. (2007). "The Habitability of Super-Earths in Gliese 581". 476. Astronomy & Astrophysics: 1365–1371. Bibcode:2007A&A...476.1365VPDF. {{cite journal}}: Check |bibcode= length (help); Cite journal requires |journal= (help); Unknown parameter |coauthors= ignored (|author= suggested) (help)
  20. ^ "New 'super-Earth' found in space". BBC News. 25 April 2007. Retrieved 20 October 2008.
  21. ^ a b Rincon, P.; Amos, J. (21 April 2009). "Lightest exoplanet is discovered". BBC News. Retrieved 21 April 2009.
  22. ^ p. 29, Vogt 2010.
  23. ^ "The astrophysicist who discovered Zarmina describes life on "second Earth"". 1 October 2010. Retrieved 1 October 2010.
  24. ^ "Keck Observatory discovers the first Goldilocks exoplanet" (Press release). Keck Observatory. 29 September 2010. Retrieved 29 September 2010.
  25. ^ pp. 15, 24, Vogt 2010.
  26. ^ "Existence of habitable exoplanet questioned". Science News. October 13 2010. Retrieved 2010-10-14. {{cite news}}: Check date values in: |date= (help); Unknown parameter |auctor= ignored (help)
  27. ^ "Notes for star Gl 581". The Extrasolar Planets Encyclopaedia. Retrieved 11 October 2010.
  28. ^ Lopez-Morales, M. (2006). "Limits to Transits of the Neptune-mass planet orbiting Gl 581". Publications of the Astronomical Society of the Pacific. 118: 1506–1509. doi:10.1086/508904. arXiv:astro-ph/0609255. V* HO Lib ... BY Draconis {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help) (page 2 of pre-print submitted 9 September 2006)
  29. ^ "General Catalogue of Variable Stars Query results". Sternberg Astronomical Institute. Retrieved 27 April 2009.
  30. ^ Weis, E. W. (1994). "Long term variability in dwarf M stars". American Astronomical Society. 107 (3): 1138. Bibcode:1994AJ....107.1135W. doi:10.1086/116925.
  31. ^ Bonfils page L15
  32. ^ Matthews, J. M. (2007). "MOST Exoplanet System Photometry" (PDF). p. 80. Retrieved 27 April 2009. {{cite web}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)

External links

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