GJ 1214

Last updated
GJ 1214 / Orkaria
GJ1214b (Artist's impression).jpg
This artist's impression shows how the super-Earth orbiting the nearby star GJ 1214 may look.
Credit: ESO/L. Calçada
Observation data
Epoch J2000       Equinox J2000
Constellation Ophiuchus [1]
Right ascension 17h 15m 18.93399s [2]
Declination +04° 57′ 50.0666″ [2]
Apparent magnitude  (V)14.71±0.03 [3]
Characteristics
Spectral type M4.5 [4]
Apparent magnitude  (B)16.40 [5]
Apparent magnitude  (R)14.394 ± 0.17 [5]
Apparent magnitude  (I)11.52 ± 0.03 [3]
Apparent magnitude  (J)9.750±0.024 [6]
Apparent magnitude  (H)9.094±0.024 [6]
Apparent magnitude  (K)8.782±0.020 [6]
B−V color index 1.73 [7]
V−R color index 0.9
R−I color index 2.7
Variable type planetary transit [8]
Astrometry
Radial velocity (Rv)+20.91±0.65 [2]  km/s
Proper motion (μ)RA: 580.202  mas/yr [2]
Dec.: −749.713  mas/yr [2]
Parallax (π)68.2986 ± 0.0652  mas [2]
Distance 47.75 ± 0.05  ly
(14.64 ± 0.01  pc)
Absolute magnitude  (MV)14.10
Details
Mass 0.181±0.005 [9]   M☉
Radius 0.204±0.0085 [9]   R☉
Luminosity 0.00351±0.00010 [9]   L☉
Surface gravity (log g)4.991±0.029 [8]   cgs
Temperature 3,111+69
−66 [9]   K
Metallicity [Fe/H]0.11±0.09 [9]   dex
Rotation 125±5 d [10]
Age 5–10 [11]   Gyr
Other designations
Orkaria, GJ  1214, G 139-21, LHS  3275, LSPM J1715+0457, NLTT  44431, TIC  467929202, 2MASS J17151894+0457496 [5]
Database references
SIMBAD data
Exoplanet Archive data
ARICNS data
Extrasolar Planets
Encyclopaedia 		data

GJ 1214 (sometimes Gliese 1214) is a dim M4.5 [4] red dwarf star in the constellation Ophiuchus with an apparent magnitude of 14.7. [3] It is located at a distance of 47.8 light-years (14.7 parsecs ) from Earth. [12] GJ 1214 hosts one known exoplanet. [8]

Contents

Nomenclature

The designation GJ 1214 comes from the Gliese Catalogue of Nearby Stars. This star was first included in the second edition of the catalogue, published in 1979 by Gliese and Jahreiß, hence the GJ prefix usually used for this star. [13]

In August 2022, this planetary system was included among 20 systems to be named by the third NameExoWorlds project. [14] The approved names, proposed by a team from Kenya, were announced in June 2023. GJ 1214 is named Orkaria and its planet is named Enaiposha, after the Maa words for red ochre and for a large body of water, alluding to the color of the star and likely composition of the planet. [15]

Properties

GJ 1214 is about one-fifth the radius of the Sun [16] with a surface temperature estimated to be 3,110 K (2,840 °C; 5,140 °F). [9] Its luminosity is only 0.35% that of the Sun. [9]

The estimate for the stellar radius is 15% larger than predicted by theoretical models. [8] It also shows a 1% intrinsic variability in the near-infrared probably caused by stellar spots. [3] The star is rotating slowly, with a period that is most likely an integer multiple of 53 days. It is probably at least three billion years old and a member of the old thin disk of the Milky Way. [3] Although GJ 1214 has a low to moderate level of magnetic activity, it does undergo flares and is a source of X-ray emission with a base luminosity of 7.4×1025 erg s−1. The temperature of the stellar corona is estimated to be about 3.5×106 K. [11]

In 2021–2022, the star is suspected to be in the low-activity phase of its magnetic starspot cycle. [17]

Planetary system

In mid-December 2009, a team of Harvard-Smithsonian astronomers announced the discovery of a companion extrasolar planet, GJ 1214 b, potentially composed largely of water and having the mass and diameter of a super-Earth, [8] [16] though now more often described as a mini-Neptune based on its composition. [18]

Discovered by the MEarth Project and investigated further by the HARPS spectrograph on ESO’s 3.6-metre telescope at La Silla, GJ 1214 b was the second super-Earth exoplanet for which astronomers determined the mass and radius, giving vital clues about its structure. It was also the first super-Earth around which an atmosphere was found. A search for additional planets using transit timing variations was negative. [3]

No transit-time variations have yet been found for this transit. As of 2012, "the given data does not allow us to conclude that there is a [second] planet in the mass range 0.1–5 Earth-masses and the period range 0.76–1.23 or 1.91–3.18 days." [19] The X-ray flux from the host star is estimated to have stripped 2–5.6 ME from the planet over the lifetime of the system. [11]

The GJ 1214 planetary system [20]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b / Enaiposha 8.17±0.43  M🜨 0.01490±0.000261.580404571(42) [21] <0.06388.7±0.1 ° 2.742+0.050
−0.053  R🜨

See also

Related Research Articles

<span class="mw-page-title-main">Gliese 876</span> Star in the constellation Aquarius

Gliese 876 is a red dwarf star 15.2 light-years away from Earth in the constellation of Aquarius. It is one of the closest known stars to the Sun confirmed to possess a planetary system with more than two planets, after GJ 1061, YZ Ceti, Tau Ceti, and Wolf 1061; as of 2018, four extrasolar planets have been found to orbit the star. The planetary system is also notable for the orbital properties of its planets. It is the only known system of orbital companions to exhibit a near-triple conjunction in the rare phenomenon of Laplace resonance. It is also the first extrasolar system around a normal star with measured coplanarity. While planets b and c are located in the system's habitable zone, they are giant planets believed to be analogous to Jupiter.

<span class="mw-page-title-main">Gliese 436</span> Star in the constellation Leo

Gliese 436 is a red dwarf located 31.9 light-years away in the zodiac constellation of Leo. It has an apparent visual magnitude of 10.67, which is much too faint to be seen with the naked eye. However, it can be viewed with even a modest telescope of 2.4 in (6 cm) aperture. In 2004, the existence of an extrasolar planet, Gliese 436 b, was verified as orbiting the star. This planet was later discovered to transit its host star.

<span class="mw-page-title-main">Gliese 229</span> Star in the constellation Lepus

Gliese 229 is a binary system composed of a red dwarf and the first brown dwarf seen by astronomers, 18.8 light years away in the constellation Lepus. The primary component has 58% of the mass of the Sun, 69% of the Sun's radius, and a very low projected rotation velocity of 1 km/s at the stellar equator.

<span class="mw-page-title-main">Gliese 667</span> Triple star system in the constellation Scorpius

Gliese 667 is a triple-star system in the constellation Scorpius lying at a distance of about 7.2 parsecs from Earth. All three of the stars have masses smaller than the Sun. There is a 12th-magnitude star close to the other three, but it is not gravitationally bound to the system. To the naked eye, the system appears to be a single faint star of magnitude 5.89.

<span class="mw-page-title-main">Gliese 436 b</span> Hot Neptune exoplanet orbiting Gliese 436

Gliese 436 b is a Neptune-sized exoplanet orbiting the red dwarf Gliese 436. It was the first hot Neptune discovered with certainty and was among the smallest-known transiting planets in mass and radius, until the much smaller Kepler exoplanet discoveries began circa 2010.

<span class="mw-page-title-main">Gliese 581d</span> Contested super-Earth orbiting Gliese 581

Gliese 581d is a doubtful, and frequently disputed, exoplanet candidate orbiting within the Gliese 581 system, approximately 20.4 light-years away in the Libra constellation. It was the third planet claimed in the system and the fourth or fifth in order from the star. Multiple subsequent studies found that the planetary signal in fact originates from stellar activity, and thus the planet does not exist, but this remains disputed.

Gliese 832 is a red dwarf of spectral type M2V in the southern constellation Grus. The apparent visual magnitude of 8.66 means that it is too faint to be seen with the naked eye. It is located relatively close to the Sun, at a distance of 16.2 light years and has a high proper motion of 818.16 milliarcseconds per year. Gliese 832 has just under half the mass and radius of the Sun. Its estimated rotation period is a relatively leisurely 46 days. The star is roughly 6 billion years old.

Gliese 806 is a star in the northern constellation of Cygnus, located about a degree to the southeast of the bright star Deneb. It is invisible to the naked eye with an apparent visual magnitude of +10.79. The star is located at a distance of 39.3 light years from the Sun based on stellar parallax. It is drifting closer with a radial velocity of −24.6 km/s, and is predicted to come to within 30.1 light-years in ~198,600 years. The star hosts two known planetary companions.

Gliese 676 is a 10th-magnitude wide binary system of red dwarfs that has an estimated minimum separation of 800 AU with an orbital period of greater than 20,000 years. It is located approximately 54 light years away in the constellation Ara. In 2009, a gas giant was found in orbit around the primary star, in addition to its confirmation in 2011 there was also a strong indication of a companion; the second gas giant was characterised in 2012, along with two much smaller planets.

<span class="mw-page-title-main">GJ 1214 b</span> Super-Earth orbiting GJ 1214

GJ 1214 b is an exoplanet that orbits the star GJ 1214, and was discovered in December 2009. Its parent star is 48 light-years from the Sun, in the constellation Ophiuchus. As of 2017, GJ 1214 b is the most likely known candidate for being an ocean planet. For that reason, scientists often call the planet a "waterworld".

Gliese 163 is a faint red dwarf star with multiple exoplanetary companions in the southern constellation of Dorado. Other stellar catalog names for it include HIP 19394 and LHS 188. It is too faint to be visible to the naked eye, having an apparent visual magnitude of 11.79 and an absolute magnitude of 10.91. This system is located at a distance of 49.4 light-years from the Sun based on parallax measurements. Judging by its space velocity components, it is most likely a thick disk star.

Gliese 221, also known as BD-06 1339, is a star with an exoplanetary companion in the equatorial constellation of Orion. It is too faint to be visible to the naked eye, having an apparent visual magnitude of 9.70 and an absolute magnitude of 8.15. Using parallax measurements, the distance to this system can be estimated as 66.2 light-years. It is receding from the Sun with a radial velocity of +23 km/s. This is a high proper motion star, traversing the celestial sphere at an angular rate of 0.333″·yr−1.

Gliese 754 is a dim star in the southern constellation of Telescopium. It has an apparent visual magnitude of 12.25, which requires a telescope to view. The star is located at a distance of 19.3 light-years from the Sun based on parallax, and it is drifting further away with a radial velocity of +7 km/s. It is one of the hundred closest stars to the Solar System. Calculations of its orbit around the Milky Way showed that it is eccentric, and indicate that it might be a thick disk object.

Gliese 251, also known as HIP 33226 or HD 265866, is a star located about 18 light years away from the Solar System. Located in the constellation of Gemini, it is the nearest star in this constellation. It is located near the boundary with Auriga, 49 arcminutes away from the bright star Theta Geminorum; due to its apparent magnitude of +9.89 it cannot be observed with the naked eye. The closest star to Gliese 251 is QY Aurigae, which is located 3.5 light years away.

<span class="mw-page-title-main">GJ 3470 b</span> Hot Neptune orbiting GJ 3470

GJ 3470 b is an exoplanet orbiting the star GJ 3470, located in the constellation Cancer. With a mass of just under 14 Earth-masses and a radius approximately 4.3 times that of Earth's, it is likely something akin to Neptune despite the initially strong belief that the planet was not covered in clouds like the gas giants in the Solar System.

GJ 3470 is a red dwarf star located in the constellation of Cancer, 96 light-years away from Earth. With a faint apparent magnitude of 12.3, it is not visible to the naked eye. It hosts one known exoplanet.

<span class="mw-page-title-main">Gliese 486</span> Star in constellation of Virgo

Gliese 486, also known as Wolf 437 and formally named Gar, is a red dwarf star 26.4 light-years away in the constellation Virgo. It hosts one known exoplanet.

Gliese 367 is a red dwarf star 30.7 light-years from Earth in the constellation of Vela. It is suspected to be a variable with amplitude 0.012 stellar magnitude and period 5.16 years. A stellar multiplicity survey in 2015 failed to detect any stellar companions to Gliese 367. It hosts three known exoplanets, Gliese 367 b, c & d.

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 3 4 5 6 Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv: 2208.00211 . Bibcode:2023A&A...674A...1G. doi: 10.1051/0004-6361/202243940 . S2CID   244398875. Gaia DR3 record for this source at VizieR.
  3. 1 2 3 4 5 6 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: 1012.0518 . Bibcode:2011ApJ...736...12B. doi:10.1088/0004-637X/736/1/12. S2CID   118428858.
  4. 1 2 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: 1007.4593 . Bibcode:2010ApJ...720L.113R. doi:10.1088/2041-8205/720/1/L113. S2CID   118378322.
  5. 1 2 3 "GJ 1214". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2019-01-15.
  6. 1 2 3 Skrutskie, Michael F.; Cutri, Roc M.; Stiening, Rae; Weinberg, Martin D.; Schneider, Stephen E.; Carpenter, John M.; Beichman, Charles A.; Capps, Richard W.; Chester, Thomas; Elias, Jonathan H.; Huchra, John P.; Liebert, James W.; Lonsdale, Carol J.; Monet, David G.; Price, Stephan; Seitzer, Patrick; Jarrett, Thomas H.; Kirkpatrick, J. Davy; Gizis, John E.; Howard, Elizabeth V.; Evans, Tracey E.; Fowler, John W.; Fullmer, Linda; Hurt, Robert L.; Light, Robert M.; Kopan, Eugene L.; Marsh, Kenneth A.; McCallon, Howard L.; Tam, Robert; Van Dyk, Schuyler D.; Wheelock, Sherry L. (1 February 2006). "The Two Micron All Sky Survey (2MASS)". The Astronomical Journal. 131 (2): 1163–1183. Bibcode:2006AJ....131.1163S. doi: 10.1086/498708 . ISSN   0004-6256. S2CID   18913331. Vizier catalog entry
  7. ↑ van Altena, William F.; et al. The General Catalogue of Trigonometric Stellar Parallaxes. Yale University Observatory. ASIN   B000UG5T6Y. Vizier catalog entry
  8. 1 2 3 4 5 Charbonneau, David; et al. (2009). "A super-Earth transiting a nearby low-mass star" (PDF). Nature. 462 (7275): 891–894. arXiv: 0912.3229 . Bibcode:2009Natur.462..891C. doi:10.1038/nature08679. PMID   20016595. S2CID   4360404.
  9. 1 2 3 4 5 6 7 Pineda, J. Sebastian; Youngblood, Allison; France, Kevin (September 2021). "The M-dwarf Ultraviolet Spectroscopic Sample. I. Determining Stellar Parameters for Field Stars". The Astrophysical Journal. 918 (1): 23. arXiv: 2106.07656 . Bibcode:2021ApJ...918...40P. doi: 10.3847/1538-4357/ac0aea . S2CID   235435757. 40.
  10. ↑ Mallonn, M.; et al. (2018). "GJ 1214: Rotation period, starspots, and uncertainty on the optical slope of the transmission spectrum". Astronomy and Astrophysics. 614. A35. arXiv: 1803.05677 . Bibcode:2018A&A...614A..35M. doi:10.1051/0004-6361/201732300. S2CID   73721250.
  11. 1 2 3 Lalitha, S.; et al. (July 2014). "X-Ray Emission from the Super-Earth Host GJ 1214". The Astrophysical Journal Letters. 790 (1): 5. arXiv: 1407.2741 . Bibcode:2014ApJ...790L..11L. doi:10.1088/2041-8205/790/1/L11. S2CID   118774018. L11.
  12. ↑ Anglada-Escudé, Guillem; Rojas-Ayala, Bárbara; Boss, Alan P.; Weinberger, Alycia J.; Lloyd, James P. (2012). "GJ 1214b revised. Improved trigonometric parallax, stellar parameters, orbital solution, and bulk properties for the super-Earth GJ 1214b". Astronomy & Astrophysics. 551: A48. arXiv: 1210.8087v3 . Bibcode:2013A&A...551A..48A. doi:10.1051/0004-6361/201219250. S2CID   55117987.
  13. ↑ "Dictionary of Nomenclature of Celestial Objects". Centre de données astronomiques de Strasbourg . Retrieved 4 May 2023.
  14. ↑ "List of ExoWorlds 2022". nameexoworlds.iau.org. IAU. 8 August 2022. Retrieved 27 August 2022.
  15. ↑ "2022 Approved Names". nameexoworlds.iau.org. IAU . Retrieved 7 June 2023.
  16. 1 2 David A. Aguilar (2009-12-16). "Astronomers Find Super-Earth Using Amateur, Off-the-Shelf Technology". Harvard-Smithsonian Center for Astrophysics. Retrieved March 21, 2024.
  17. ↑ Henry, Gregory W.; Bean, Jacob L. (2023), C14 Automatic Imaging Telescope Photometry of GJ 1214, arXiv: 2302.07874
  18. ↑ Brennan, Pat (10 May 2023). "NASA's Webb Takes Closest Look Yet at Mysterious Planet". NASA . Retrieved 10 May 2023.
  19. ↑ Kennet B. W. Harpsøe; et al. (2012). "The transiting system GJ1214: high-precision defocused transit observations and a search for evidence of transit timing variation". Astronomy & Astrophysics. 549: A10. arXiv: 1207.3064 . Bibcode:2013A&A...549A..10H. doi:10.1051/0004-6361/201219996. S2CID   53418632.
  20. ↑ Cloutier, Ryan; Charbonneau, David; Deming, Drake; Bonfils, Xavier; Astudillo-Defru, Nicola (2021), "A More Precise Mass for GJ 1214 b and the Frequency of Multiplanet Systems Around Mid-M Dwarfs", The Astronomical Journal, 162 (5): 174, arXiv: 2107.14732 , Bibcode:2021AJ....162..174C, doi: 10.3847/1538-3881/ac1584 , S2CID   236635146
  21. ↑ Kokori, A.; et al. (14 February 2023). "ExoClock Project. III. 450 New Exoplanet Ephemerides from Ground and Space Observations". The Astrophysical Journal Supplement Series. 265 (1) 4. arXiv: 2209.09673 . Bibcode: 2023ApJS..265....4K . doi: 10.3847/1538-4365/ac9da4 . Vizier catalog entry
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.