Gliese 486

Last updated
Gliese 486 / Gar
Gliese486 SDSS9.png
Observation data
Epoch J2000       Equinox J2000
Constellation Virgo
Right ascension 12h 47m 56.62457s [1]
Declination +09° 45′ 05.0357″ [1]
Apparent magnitude  (V)11.395
Characteristics
Evolutionary stage main sequence
Spectral type M3.5V [2]
Astrometry
Radial velocity (Rv)19.20±0.17 [1]  km/s
Proper motion (μ)RA: −1008.267  mas/yr [1]
Dec.: −460.034  mas/yr [1]
Parallax (π)123.7756 ± 0.0329  mas [1]
Distance 26.351 ± 0.007  ly
(8.079 ± 0.002  pc)
Details [3]
Mass 0.323±0.015  M☉
Radius 0.328±0.011  R☉
Luminosity 0.01210±0.00023  L☉
Temperature 3340±54  K
Metallicity [Fe/H]−0.15±0.13 [4]   dex
Rotation 49.9±5.5 d [4]
Rotational velocity (v sin i)<2 [5]  km/s
Age 1-8 [4]   Gyr
Other designations
Gar, GJ  486, HIP  62452, Wolf  437, TOI-1827, TYC  882-1111-1, 2MASS J12475664+0945050 [6]
Database references
SIMBAD data

Gliese 486, also known as Wolf 437 and formally named Gar, is a red dwarf star 26.4 light-years (8.1 parsecs ) away in the constellation Virgo. It hosts one known exoplanet. [3]

Contents

Nomenclature

The designation Gliese 486 comes from the Gliese Catalogue of Nearby Stars. This was the 486th star listed in the first edition of the catalogue.

In August 2022, this planetary system was included among 20 systems to be named by the third NameExoWorlds project. [7] The approved names, proposed by a team from Spain, were announced in June 2023. Gliese 486 is named Gar and its planet is named Su, after the Basque words for "flame" and "fire". [8]

Properties

Gliese 486 has a surface temperature of 3340±54 K. Gliese 486 is similar to the Sun in its concentration of heavy elements, with a metallicity Fe/H index of 0.07±0.16. It was suspected to be a flare star, [9] although measurements available in 2019 did not reveal any flares. [10] The chemical makeup of the star is unremarkable and consistent with solar abundances or being slightly metal-poor. [4]

The star has an unremarkable magnetic field in the chromosphere of about 1.6 kilogauss. [5] It is rotating very slowly and is likely to be very old, belonging kinematically to the old thin disk of the Milky Way. [11]

Multiplicity surveys did not detect any stellar companions to Gliese 486 as of 2020. [12]

Planetary system

Artistic impression of the surface of the hot super-Earth Gliese 486b. Gliese486b HotSuperEarth.png
Artistic impression of the surface of the hot super-Earth Gliese 486b.

In 2021, one planet, named Gliese 486 b, was discovered on a tight, circular orbit. [3] It represents a rare class of rocky exoplanet suitable for spectroscopic characterization in the near future [13] by the James Webb Space Telescope. [14] As of 2022, no hydrogen or steam dominated atmosphere was detected, although a secondary planetary atmosphere with a higher molecular weight remains a possibility. [15] Observations by JWST announced in 2023 detected signs of water vapor, but it is unclear if this is from the planet's atmosphere or from its host star. [16] [17]

The Gliese 486 planetary system [3]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b / Su2.82+0.11
−0.12  M🜨 		0.01734+0.00026
−0.00027		1.467119+0.000031
−0.000030		<0.0588.4+1.1
−1.4 ° 		1.305+0.063
−0.067  R🜨

Related Research Articles

<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 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.

Gliese 849, or GJ 849, is a small, solitary star in the equatorial constellation of Aquarius. It has a reddish hue and is invisible to the naked eye with an apparent visual magnitude of 10.41. The distance to this star is 28.8 light-years based on parallax, but it is drifting closer to the Sun with a radial velocity of −15.3 km/s. It has a pair of confirmed gas giant companions.

Gliese 86 is a K-type main-sequence star approximately 35 light-years away in the constellation of Eridanus. It has been confirmed that a white dwarf orbits the primary star. In 1998 the European Southern Observatory announced that an extrasolar planet was orbiting the star.

Gliese 176 is a small star with an orbiting exoplanet in the constellation of Taurus. With an apparent visual magnitude of 9.95, it is too faint to be visible to the naked eye. It is located at a distance of 30.9 light years based on parallax measurements, and is drifting further away with a heliocentric radial velocity of 26.4 km/s.

HAT-P-12 is a magnitude 13 low-metallicity K dwarf star approximately 463 light years away in the constellation Canes Venatici, which hosts one known exoplanet.

Gliese 433 is a dim red dwarf star with multiple exoplanetary companions, located in the equatorial constellation of Hydra. The system is located at a distance of 29.6 light-years from the Sun based on parallax measurements, and it is receding with a radial velocity of +18 km/s. Based on its motion through space, this is an old disk star. It is too faint to be viewed with the naked eye, having an apparent visual magnitude of 9.81 and an absolute magnitude of 10.07.

<span class="mw-page-title-main">GJ 1214</span> Star in the constellation Ophiuchus

GJ 1214 is a dim M4.5 red dwarf star in the constellation Ophiuchus with an apparent magnitude of 14.7. It is located at a distance of 47.8 light-years from Earth. GJ 1214 hosts one known exoplanet.

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 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 880 is a red dwarf star in the northern constellation of Pegasus that may host an exoplanetary companion. No stellar companions to Gliese 880 have been discovered as of 2020.

HAT-P-26 is a K-type main-sequence star about 466 light-years away. A survey in 2015 did not find any stellar companions in orbit around it, although a red dwarf companion with a temperature 4000+100
−350 K is suspected on wide orbit.

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.

WASP-63 or Kosjenka, also known as CD-38 2551, is a single star with an exoplanetary companion in the southern constellation of Columba. It is too faint to be visible with the naked eye, having an apparent visual magnitude of 11.1. The distance to this system is approximately 942 light-years based on parallax measurements, but it is drifting closer with a radial velocity of −24 km/s.

WASP-69, also named Wouri, is a K-type main-sequence star 164 light-years away. Its surface temperature is 4782±15 K. WASP-69 is slightly enriched in heavy elements compared to the Sun, with a metallicity Fe/H index of 0.10±0.01, and is much younger than the Sun at 2 billion years. The data regarding starspot activity of WASP-69 are inconclusive, but spot coverage of the photosphere may be very high.

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.

Gliese 514, also known as BD+11 2576 or HIP 65859, is a M-type main-sequence star, in the constellation Virgo 24.85 light-years away from the Sun. The proximity of Gliese 514 to the Sun was known exactly since 1988.

LHS 3844 is a red dwarf star located 48.5 light-years away from the Solar System in the constellation of Indus. The star has about 15% the mass and 19% the radius of the Sun. It is a relatively inactive red dwarf with a slow rotation period of about 128 days, though UV flares have been observed. LHS 3844 is orbited by one known exoplanet.

L 168-9 is a red dwarf star located 82.1 light-years away from the Solar System in the constellation of Tucana. The star has about 62% the mass and 60% the radius of the Sun. It has a temperature of 3,800 K and a rotation period of 29.8 days. L 168-9 is orbited by one known exoplanet.

References

  1. 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.
  2. ↑ Bozhinova, I.; Helling, Ch.; Scholz, A. (2014), "Planetary host stars: Evaluating uncertainties in cool model atmospheres", Monthly Notices of the Royal Astronomical Society, 450: 160–182, arXiv: 1405.5416 , Bibcode:2015MNRAS.450..160B, doi:10.1093/mnras/stv613
  3. 1 2 3 4 Trifonov, T.; et al. (2021), "A nearby transiting rocky exoplanet that is suitable for atmospheric investigation", Science, 371 (6533): 1038–1041, arXiv: 2103.04950 , Bibcode:2021Sci...371.1038T, doi:10.1126/science.abd7645, PMID   33674491, S2CID   232124642
  4. 1 2 3 4 Caballero, J. A.; et al. (2022), "A detailed analysis of the Gl 486 planetary system", Astronomy & Astrophysics, 665: A120, arXiv: 2206.09990 , Bibcode:2022A&A...665A.120C, doi:10.1051/0004-6361/202243548, S2CID   249889232
  5. 1 2 Moutou, Claire; Hébrard, Élodie M.; Morin, Julien; Malo, Lison; Fouqué, Pascal; Torres-Rivas, Andoni; Martioli, Eder; Delfosse, Xavier; Artigau, Étienne; Doyon, René (2017), "SPIRou input catalogue: Activity, rotation and magnetic field of cool dwarfs", Monthly Notices of the Royal Astronomical Society, 472 (4): 4563–4586, arXiv: 1709.01650 , Bibcode:2017MNRAS.472.4563M, doi:10.1093/mnras/stx2306
  6. ↑ "Wolf 437". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2021-03-10.
  7. ↑ "List of ExoWorlds 2022". nameexoworlds.iau.org. IAU. 8 August 2022. Retrieved 27 August 2022.
  8. ↑ "2022 Approved Names". nameexoworlds.iau.org. IAU . Retrieved 7 June 2023.
  9. ↑ O'Donoghue, D.; Koen, C.; Kilkenny, D.; Stobie, R. S.; Koester, D.; Bessell, M. S.; Hambly, N.; MacGillivray, H. (2003), "The DA+d Me eclipsing binary EC13471-1258: its cup runneth over ... Just", Monthly Notices of the Royal Astronomical Society, 345 (2): 506–528, arXiv: astro-ph/0307144 , Bibcode:2003MNRAS.345..506O, doi:10.1046/j.1365-8711.2003.06973.x, S2CID   17408072
  10. ↑ Vida, Krisztián; Leitzinger, Martin; Kriskovics, Levente; Seli, Bálint; Odert, Petra; Kovács, Orsolya Eszter; Korhonen, Heidi; Van Driel-Gesztelyi, Lidia (2019), "The quest for stellar coronal mass ejections in late-type stars", Astronomy & Astrophysics, 623: A49, arXiv: 1901.04229 , doi:10.1051/0004-6361/201834264, S2CID   119095055
  11. ↑ Browning, Matthew K.; Basri, Gibor; Marcy, Geoffrey W.; West, Andrew A.; Zhang, Jiahao (2010), "Rotation and Magnetic Activity in a Sample of M-Dwarfs", The Astronomical Journal, 139 (2): 504, Bibcode:2010AJ....139..504B, doi: 10.1088/0004-6256/139/2/504 , S2CID   121835145
  12. ↑ Lamman, Claire; Baranec, Christoph; Berta-Thompson, Zachory K.; Law, Nicholas M.; Schonhut-Stasik, Jessica; Ziegler, Carl; Salama, Maïssa; Jensen-Clem, Rebecca; Duev, Dmitry A.; Riddle, Reed; Kulkarni, Shrinivas R.; Winters, Jennifer G.; Irwin, Jonathan M. (2020), "Robo-AO M-dwarf Multiplicity Survey: Catalog", The Astronomical Journal, 159 (4): 139, arXiv: 2001.05988 , Bibcode:2020AJ....159..139L, doi: 10.3847/1538-3881/ab6ef1 , S2CID   210718832
  13. ↑ Hot Super-Earth Discovered 26 Light-Years Away
  14. ↑ Newfound exoplanet could be 'Rosetta Stone' for studies of alien atmospheres
  15. ↑ Ridden-Harper, Andrew; Nugroho, Stevanus; Flagg, Laura; Jayawardhana, Ray; Turner, Jake D.; Ernst de Mooij; MacDonald, Ryan; Deibert, Emily; Tamura, Motohide; Kotani, Takayuki; Hirano, Teruyuki; Kuzuhara, Masayuki; Omiya, Masashi; Kusakabe, Nobuhiko (2023), "High-resolution Transmission Spectroscopy of the Terrestrial Exoplanet GJ 486b", The Astronomical Journal, 165 (4): 170, arXiv: 2212.11816 , Bibcode:2023AJ....165..170R, doi: 10.3847/1538-3881/acbd39
  16. ↑ Moran, Sarah E.; Stevenson, Kevin B.; et al. (May 2023). "High Tide or Rip-Tide on the Cosmic Shoreline? A Water-Rich Atmosphere or Stellar Contamination for the Warm Super-Earth GJ 486b from JWST Observations". The Astrophysical Journal Letters . 948 (1): L11. arXiv: 2305.00868 . Bibcode:2023ApJ...948L..11M. doi: 10.3847/2041-8213/accb9c .
  17. ↑ "Webb Finds Water Vapor, But From a Rocky Planet or Its Star?". webbtelescope.org. STScI. 1 May 2023. Retrieved 1 May 2023.
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.