Gliese 1214 b

GJ 1214 b
Exoplanet List of exoplanets

Artist's impression of GJ 1214 b (foreground), illuminated by the red light of its parent star (center).
Parent star
Star GJ 1214
Constellation Ophiuchus[1]
Right ascension (α) 17h 15m 18.942s[2]
Declination (δ) +04° 57′ 49.69″[2]
Apparent magnitude (mV) 14.71±0.03[3]
Distance42±3[4] ly
(13.0±0.9[4] pc)
Spectral type M4.5[5]
Mass (m) 0.157[6] M☉
Radius (r) 0.2064+0.0086
−0.0096[3] R☉
Temperature (T) 3026±130[6] K
Age 6 Gyr
Orbital elements
Semi-major axis(a) 0.0143±0.0019 AU
(2.14 Gm)
    1.1 mas
Eccentricity (e) < 0.27
Orbital period(P) 1.58040456±0.00000016[7] d
Orbital speed (υ) 99 km/s
Inclination (i) 88.62+0.36
−0.28°
Time of transit (Tt) 2454999.712703±0.000126 JD
Physical characteristics
Mass(m)6.55±0.98 (HARPS)[6] M⊕
Radius(r)2.678±0.13 R⊕
Density(ρ)1870±400 kg m−3
Stellar flux(F⊙)16 ⊕
Surface gravity(g)0.91 g
Temperature (T) 393–555 K (120–282 °C; 248–539 °F) (equilibrium)[6]
Discovery information
Discovery date December 16, 2009
Discoverer(s) David Charbonneau, et al.[6]
Discovery method Transit (MEarth Project)
Other detection methods Radial velocity
Discovery site Fred Lawrence Whipple Observatory
Discovery status Published[6]
Database references
Extrasolar Planets
Encyclopaedia		data
SIMBADdata
Exoplanet Archivedata
Open Exoplanet Cataloguedata

Gliese 1214 b[8] (often shortened to GJ 1214 b) is an exoplanet that orbits the star Gliese 1214, and was discovered in December 2009. Its parent star is 42 light-years from the Sun, in the constellation Ophiuchus. As of 2015, GJ 1214 b is the most likely known candidate for being an ocean planet.[9][10] For that reason, scientists have nicknamed the planet "the waterworld".[11]

It is a super-Earth, meaning it is larger than Earth but is significantly smaller (in mass and radius) than the gas giants of the Solar System. After COROT-7b, it was the second super-Earth to be known[6] and is the first of a new class of planets with small size and relatively low density.[12] GJ 1214 b is also significant because its parent star is relatively near the Sun and because it transits (crosses in front of) that parent star, which allows the planet's atmosphere to be studied using spectroscopic methods.[6]

In December 2013, NASA reported that clouds may have been detected in the atmosphere of GJ 1214 b.[13][14][15][16]

Detection

GJ 1214 b was first detected by the MEarth Project, which searches for the small drops in brightness that can occur when an orbiting planet briefly passes in front of its parent star. In early 2009, the astronomers running the project noticed that the star GJ 1214 appeared to show drops in brightness of that sort. They then observed the star more closely and confirmed that it dimmed by roughly 1.5% every 1.58 days. Follow-up radial-velocity measurements were then made with the HARPS spectrograph on the ESO's 3.6-meter telescope at La Silla, Chile; those measurements succeeded in providing independent evidence for the reality of the planet. A paper was then published in Nature announcing the planet and giving estimates of its mass, radius, and orbital parameters.[6]

Features

GJ 1214 b is about 2.7 times Earth's diameter and is almost seven times as massive.[17] Neptune and Earth are shown here for size comparison.

The radius of GJ 1214 b can be inferred from the amount of dimming seen when the planet crosses in front of its parent star as viewed from Earth. The mass of the planet can be inferred from sensitive observations of the parent star's radial velocity, measured through small shifts in stellar spectral lines due to the Doppler effect.[6] Given the planet's mass and radius, its density can be calculated. Through a comparison with theoretical models, the density in turn provides limited but highly useful information about the composition and structure of the planet.[6]

The newly discovered super-Earth orbiting the nearby star GJ 1214.
This artist's impression shows how GJ 1214 b may look as it transits its parent star. It is the second super-Earth for which astronomers have determined the mass and radius, giving vital clues about its structure.

Due to the relatively small size of GJ 1214 b's parent star, it is feasible to perform spectroscopic observations during planetary transits. By comparing the observed spectrum before and during transits, the spectrum of the planetary atmosphere can be inferred. In December 2010, a study was published showing the spectrum to be largely featureless over the wavelength range of 750–1000 nm. Because a thick and cloud-free hydrogen-rich atmosphere would have produced detectable spectral features, such an atmosphere appears to be ruled out. Although no clear signs were observed of water vapor or any other molecule, the authors of the study believe the planet may have an atmosphere composed mainly of water vapor. Another possibility is that there may be a thick layer of high clouds, which absorbs the starlight.[18] Further observations are necessary to determine the composition of its atmosphere.

Because of the estimated old age of the planetary system and the calculated hydrodynamic escape rate of 9×105 kg s−1, scientists conclude that there has been a significant atmospheric loss during the lifetime of the planet and any current atmosphere cannot be primordial.[6]

GJ 1214 b may be cooler than any other known transiting planet prior to the discovery of Kepler-16b in 2011 by the Kepler mission. Its equilibrium temperature could be between approximately 393–555 K (120–282 °C or 248–540 °F), depending on how much of the star's radiation is reflected back into space.[6][19]

Speculation based on planetary models

While very little is known about GJ 1214 b, that does not prevent wild speculation in the press. On the basis of planetary models [20] it has been suggested that GJ 1214 b has a relatively thick gaseous envelope.[12] It is possible to propose structures by assuming different compositions, guided by scenarios for the formation and evolution of the planet.[12] GJ 1214 b could be a rocky planet with an outgassed hydrogen-rich atmosphere, a mini-Neptune, or an ocean planet.[12] If it is a water world, it could possibly be thought of as a bigger and hotter version of Jupiter's Galilean moons.[12] While no scientist has stated to believe GJ 1214 b is an ocean planet, if GJ 1214 b is assumed to be an ocean planet,[20] i.e. the interior is assumed to be composed primarily of a water core surrounded by more water, proportions of the total mass consistent with the mass and radius are ~25% rock and ~75% water, covered by a thick envelope of gases such as hydrogen and helium (~0.05%).[6][19] Water planets could result from inward planetary migration and originate as protoplanets that formed from volatile ice-rich material beyond the snow-line but that never attained masses sufficient to accrete large amounts of H/He nebular gas.[12] Because of the varying pressure at depth, models of a water world include "steam, liquid, superfluid, high-pressure ices, and plasma phases" of water.[12] Some of the solid-phase water could be in the form of ice VII.[19]

See also

References

  1. ↑ Roman, Nancy G. (1987). "Identification of a Constellation From a Position". Publications of the Astronomical Society of the Pacific. 99 (617): 695–699. Bibcode:1987PASP...99..695R. doi:10.1086/132034. Vizier query form
  2. 1 2 Skrutskie, M. F.; et al. (2006). "The Two Micron All Sky Survey (2MASS)". The Astronomical Journal. 131 (2): 1163–1183. Bibcode:2006AJ....131.1163S. doi:10.1086/498708. Vizier catalog entry
  3. 1 2 Berta, Zachory K.; et al. (2011). "The GJ1214 Super-Earth System: Stellar Variability, New Transits, and a Search for Additional Planets". The Astrophysical Journal. 736 (1). 12. arXiv:1012.0518Freely accessible. Bibcode:2011ApJ...736...12B. doi:10.1088/0004-637X/736/1/12.
  4. 1 2 van Altena, William F.; et al. The General Catalogue of Trigonometric Stellar Parallaxes. Yale University Observatory. ASIN B000UG5T6Y.Vizier catalog entry
  5. ↑ Rojas-Ayala, Bárbara; et al. (2010). "Metal-rich M-Dwarf Planet Hosts: Metallicities with K-band Spectra". The Astrophysical Journal Letters. 720 (1): L113–L118. arXiv:1007.4593Freely accessible. Bibcode:2010ApJ...720L.113R. doi:10.1088/2041-8205/720/1/L113.
  6. 1 2 3 4 5 6 7 8 9 10 11 12 13 14 Charbonneau, David; et al. (2009). "A super-Earth transiting a nearby low-mass star". Nature. 462 (7275): 891–894. arXiv:0912.3229Freely accessible. Bibcode:2009Natur.462..891C. doi:10.1038/nature08679. PMID 20016595.
  7. ↑ Kennet B. W. Harpsøe; et al. (2012). "The Transiting System GJ1214". Astronomy & Astrophysics. 549: A10. arXiv:1207.3064Freely accessible. Bibcode:2013A&A...549A..10H. doi:10.1051/0004-6361/201219996.
  8. ↑ Rein, Hanno; et al. "Open Exoplanet Catalogue - Gliese 1214 b". Open Exoplanet Catalogue. Retrieved 2 January 2014.
  9. ↑ David Charbonneau; Zachory K. Berta; Jonathan Irwin; Christopher J. Burke; et al. (2009). "A super-Earth transiting a nearby low-mass star". Nature. 462 (17 December 2009): 891–894. arXiv:0912.3229Freely accessible. Bibcode:2009Natur.462..891C. doi:10.1038/nature08679. PMID 20016595. Retrieved 2009-12-15.
  10. ↑ Kuchner, Seager; Hier-Majumder, M.; Militzer, C. A. (2007). "Mass–radius relationships for solid exoplanets". The Astrophysical Journal. 669 (2): 1279–1297. arXiv:0707.2895Freely accessible. Bibcode:2007ApJ...669.1279S. doi:10.1086/521346.
  11. ↑ "10 Real Planets That Are Stranger Than Science Fiction". Retrieved 2015-06-13.
  12. 1 2 3 4 5 6 7 Rogers, L.A.; Seager, S. (2009-12-16). "Three Possible Origins for the Gas Layer on GJ 1214b". The Astrophysical Journal (abstract). 716 (2): 1208–1216. arXiv:0912.3243Freely accessible. Bibcode:2010ApJ...716.1208R. doi:10.1088/0004-637X/716/2/1208.
  13. ↑ Harrington, J.D.; Weaver, Donna; Villard, Ray (December 31, 2013). "Release 13-383 - NASA's Hubble Sees Cloudy Super-Worlds With Chance for More Clouds". NASA. Retrieved January 1, 2014.
  14. ↑ Moses, Julianne (January 1, 2014). "Extrasolar planets: Cloudy with a chance of dustballs". Nature. 505 (7481): 31–32. Bibcode:2014Natur.505...31M. doi:10.1038/505031a. PMID 24380949. Retrieved January 1, 2014.
  15. ↑ Knutson, Heather; et al. (January 1, 2014). "A featureless transmission spectrum for the Neptune-mass exoplanet GJ 436b". Nature. 505 (7481): 66–68. arXiv:1401.3350Freely accessible. Bibcode:2014Natur.505...66K. doi:10.1038/nature12887. PMID 24380953. Retrieved January 1, 2014.
  16. ↑ Kreidberg, Laura; et al. (January 1, 2014). "Clouds in the atmosphere of the super-Earth exoplanet GJ 1214b". Nature. 505 (7481): 69–72. arXiv:1401.0022Freely accessible. Bibcode:2014Natur.505...69K. doi:10.1038/nature12888. PMID 24380954. Retrieved January 1, 2014.
  17. ↑ "Hubble Reveals a New Class of Extrasolar Planet". ESA/Hubble Press Release. Retrieved 22 February 2012.
  18. ↑ Bean, Jacob L.; Kempton, Eliza Miller-Ricci; Homeier, Derek (2010). "A ground-based transmission spectrum of the super-Earth exoplanet GJ 1214b". Nature. 468 (7324): 669–672. arXiv:1012.0331Freely accessible. Bibcode:2010Natur.468..669B. doi:10.1038/nature09596.
  19. 1 2 3 David A. Aguilar (2009-12-16). "Astronomers Find Super-Earth Using Amateur, Off-the-Shelf Technology". Harvard-Smithsonian Center for Astrophysics. Retrieved December 16, 2009.
  20. 1 2 Seager, S.; Kuchner, M.; Hier-Majumder, C. A.; Militzer, B. (2007). "Mass–radius relationships for solid exoplanets". The Astrophysical Journal. 669 (2): 1279–1297. arXiv:0707.2895Freely accessible. Bibcode:2007ApJ...669.1279S. doi:10.1086/521346.

External links

Media related to Gliese 1214 b at Wikimedia Commons

Coordinates: 17h 15m 18.94s, +4° 57′ 49.7″

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