Gliese 682

Gliese 682
Gliese 682 is located in the constellation Scorpius
Gliese 682 is located in the constellation Scorpius
Gliese 682
Location of Gliese 682 in the constellation Scorpius

Observation data
Epoch J2000      Equinox
Constellation Scorpius
Right ascension 17h 37m 03.6655s[1]
Declination −44° 19′ 09.166″[1]
Apparent magnitude (V) 10.94[2]
Characteristics
Spectral type M3.5V[3]
Apparent magnitude (B) ~12.61[4]
Apparent magnitude (V) ~10.96[4]
Apparent magnitude (J) 6.544 ±0.023[4]
Apparent magnitude (H) 5.917 ±0.038[4]
Apparent magnitude (K) 5.606 ±0.020[4]
Astrometry
Radial velocity (Rv)−34.90±0.30[1] km/s
Proper motion (μ) RA: −705.945±0.035 mas/yr[1]
Dec.: −938.080±0.021 mas/yr[1]
Parallax (π)199.6944 ± 0.0312 mas[1]
Distance16.333 ± 0.003 ly
(5.0077 ± 0.0008 pc)
Absolute magnitude (MV)12.4[5]
Details
Mass0.27[3] M☉
Radius0.30[2] R☉
Luminosity0.008118[3] L☉
Surface gravity (log g)4.95[6] cgs
Temperature3,237[2] K
Metallicity [Fe/H]0.05±0.09[6] dex
Rotational velocity (v sin i)3.42[7] km/s
Age6.4±4.3[6] Gyr
Other designations
CD−44 11909, GJ 682, LHS 451, LFT 1358, HIP 86214, PLX 3992.
Database references
SIMBADstar
planet b
planet c
Exoplanet Archivedata
ARICNSdata

Gliese 682 or GJ 682 is a red dwarf. It is listed as the 53rd-nearest known star system to the Sun,[8] being 16.3 light years away from the Earth. Even though it is close by, it is dim with a magnitude of 10.95 and thus requires a telescope to be seen. It is located in the constellation of Scorpius, near the bright star Theta Scorpii.[4] The star is in a crowded region of sky near the Galactic Center, and so appears to be near a number of deep-sky objects from the Solar System's perspective. The star is only 0.5 degrees from the much more distant globular cluster NGC 6388.

Search for planets

The Gliese 682 planetary system[9]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b (unconfirmed) >4.4 M⊕ 0.08 17.48 0.08 — —
c (unconfirmed) >8.7 M⊕ 0.18 57.32 0.10 — —

Two candidate planets were detected orbiting Gliese 682 in 2014, one of which would be in the habitable zone.[9][10] However, a 2020 study did not find these planets and concluded that the radial velocity signals were probably caused by stellar activity.[11]

See also

References

  1. ^ a b c d e 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. ^ a b c Suissa, Gabrielle; Mandell, Avi M.; Wolf, Eric T.; Villanueva, Geronimo L.; Fauchez, Thomas; Kopparapu, Ravi Kumar (2020). "Dim Prospects for Transmission Spectra of Ocean Earths around M Stars". The Astrophysical Journal. 891 (1): 58. arXiv:1912.08235. Bibcode:2020ApJ...891...58S. doi:10.3847/1538-4357/ab72f9. S2CID 209405220.
  3. ^ a b c Martínez-Rodríguez, Héctor; Caballero, José Antonio; Cifuentes, Carlos; Piro, Anthony L.; Barnes, Rory (2019). "Exomoons in the Habitable Zones of M Dwarfs". The Astrophysical Journal. 887 (2): 261. arXiv:1910.12054. Bibcode:2019ApJ...887..261M. doi:10.3847/1538-4357/ab5640. S2CID 204904780.
  4. ^ a b c d e f "LHS 451 -- High proper-motion Star". Centre de Données astronomiques de Strasbourg. Retrieved 2009-12-14.
  5. ^ Boro Saikia, S.; Marvin, C. J.; Jeffers, S. V.; Reiners, A.; Cameron, R.; Marsden, S. C.; Petit, P.; Warnecke, J.; Yadav, A. P. (2018). "Chromospheric activity catalogue of 4454 cool stars. Questioning the active branch of stellar activity cycles". Astronomy and Astrophysics. 616: 616. arXiv:1803.11123. Bibcode:2018A&A...616A.108B. doi:10.1051/0004-6361/201629518. S2CID 118915212.
  6. ^ a b c Maldonado, J.; Micela, G.; Baratella, M.; d'Orazi, V.; Affer, L.; Biazzo, K.; Lanza, A. F.; Maggio, A.; González Hernández, J. I.; Perger, M.; Pinamonti, M.; Scandariato, G.; Sozzetti, A.; Locci, D.; Di Maio, C.; Bignamini, A.; Claudi, R.; Molinari, E.; Rebolo, R.; Ribas, I.; Toledo-Padrón, B.; Covino, E.; Desidera, S.; Herrero, E.; Morales, J. C.; Suárez-Mascareño, A.; Pagano, I.; Petralia, A.; Piotto, G.; Poretti, E. (2020). "HADES RV programme with HARPS-N at TNG. XII. The abundance signature of M dwarf stars with planets". Astronomy and Astrophysics. 644: A68. arXiv:2010.14867. Bibcode:2020A&A...644A..68M. doi:10.1051/0004-6361/202039478. S2CID 225094682.
  7. ^ Hojjatpanah, S.; Figueira, P.; Santos, N. C.; Adibekyan, V.; Sousa, S. G.; Delgado-Mena, E.; Alibert, Y.; Cristiani, S.; González Hernández, J. I.; Lanza, A. F.; Di Marcantonio, P.; Martins, J. H. C.; Micela, G.; Molaro, P.; Neves, V.; Oshagh, M.; Pepe, F.; Poretti, E.; Rojas-Ayala, B.; Rebolo, R.; Suárez Mascareño, A.; Zapatero Osorio, M. R. (2019). "Catalog for the ESPRESSO blind radial velocity exoplanet survey". Astronomy and Astrophysics. 629: A80. arXiv:1908.04627. Bibcode:2019A&A...629A..80H. doi:10.1051/0004-6361/201834729. S2CID 199552090.
  8. ^ Reylé, Céline; Jardine, Kevin; Fouqué, Pascal; Caballero, Jose A.; Smart, Richard L.; Sozzetti, Alessandro (30 April 2021). "The 10 parsec sample in the Gaia era". Astronomy & Astrophysics. 650: A201. arXiv:2104.14972. Bibcode:2021A&A...650A.201R. doi:10.1051/0004-6361/202140985. S2CID 233476431. Data available at https://gruze.org/10pc/
  9. ^ a b Tuomi, M.; et al. (2014). "Bayesian search for low-mass planets around nearby M dwarfs - estimates for occurrence rate based on global detectability statistics". Monthly Notices of the Royal Astronomical Society. 441 (2): 1545. arXiv:1403.0430. Bibcode:2014MNRAS.441.1545T. doi:10.1093/mnras/stu358. S2CID 32965505.
  10. ^ "The Habitable Exoplanets Catalog". Planetary Habitability Laboratory. University of Puerto Rico at Arecibo. Retrieved 7 October 2020.
  11. ^ Feng, Fabo; Butler, R. Paul; Shectman, Stephen A.; Crane, Jeffrey D.; Vogt, Steve; Chambers, John; Jones, Hugh R. A.; Wang, Sharon Xuesong; Teske, Johanna K.; Burt, Jenn; Díaz, Matías R.; Thompson, Ian B. (8 January 2020). "Search for Nearby Earth Analogs. II. Detection of Five New Planets, Eight Planet Candidates, and Confirmation of Three Planets around Nine Nearby M Dwarfs". The Astrophysical Journal Supplement Series. 246 (1): 11. arXiv:2001.02577. Bibcode:2020ApJS..246...11F. doi:10.3847/1538-4365/ab5e7c. S2CID 210064560.