Astronomy:Gliese 682
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Short description: Star in the constellation Scorpius
Coordinates: 
17h 37m 03.6613s, −44° 19′ 09.18″
  Gliese 682 Location of Gliese 682 in the constellation Scorpius | |
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Scorpius[1] |
| Right ascension | 17h 37m 03.6655s[2] |
| Declination | −44° 19′ 09.166″[2] |
| Apparent magnitude (V) | 10.94[3] |
| Characteristics | |
| Spectral type | M3.5V[4] |
| Apparent magnitude (B) | ~12.61[5] |
| Apparent magnitude (V) | ~10.96[5] |
| Apparent magnitude (J) | 6.544 ±0.023[5] |
| Apparent magnitude (H) | 5.917 ±0.038[5] |
| Apparent magnitude (K) | 5.606 ±0.020[5] |
| Astrometry | |
| Radial velocity (Rv) | −34.90±0.30[2] km/s |
| Proper motion (μ) | RA: −705.945±0.035[2] mas/yr Dec.: −938.080±0.021[2] mas/yr |
| Parallax (π) | 199.6944 ± 0.0312[2] mas |
| Distance | 16.333 ± 0.003 ly (5.0077 ± 0.0008 pc) |
| Absolute magnitude (MV) | 12.4[6] |
| Details | |
| Mass | 0.27[4] M☉ |
| Radius | 0.30[3] R☉ |
| Luminosity | 0.008118[4] L☉ |
| Surface gravity (log g) | 4.95[7] cgs |
| Temperature | 3,237[3] K |
| Metallicity [Fe/H] | 0.05±0.09[7] dex |
| Rotational velocity (v sin i) | 3.42[8] km/s |
| Age | 6.4±4.3[7] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | star |
| planet b | |
| planet c | |
| Exoplanet Archive | data |
| ARICNS | data |
Gliese 682, also known as GJ 682, is a nearby star. It is listed as the 53rd-nearest known star system to the Sun,[9] being 16.3 light years distant. Even though it is close by, as a red dwarf, 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.[5] 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
Two candidate planets were detected orbiting Gliese 682 in 2014, one of which would be in the habitable zone.[10][11] However, a 2020 study did not find these planets and concluded that the radial velocity signals were probably caused by stellar activity.[12]
References
- ↑ Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331. doi:10.1134/S1063773712050015. Bibcode: 2012AstL...38..331A.
- ↑ 2.0 2.1 2.2 2.3 2.4 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940 Gaia DR3 record for this source at VizieR.
- ↑ 3.0 3.1 3.2 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. doi:10.3847/1538-4357/ab72f9. Bibcode: 2020ApJ...891...58S.
- ↑ 4.0 4.1 4.2 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. doi:10.3847/1538-4357/ab5640. Bibcode: 2019ApJ...887..261M.
- ↑ 5.0 5.1 5.2 5.3 5.4 5.5 "LHS 451 -- High proper-motion Star". Centre de Données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-id?Ident=GJ+682.
- ↑ Boro Saikia, S.; Marvin, C. J.; Jeffers, S. V.; Reiners, A.; Cameron, R.; Marsden, S. C.; Petit, P.; Warnecke, J. et al. (2018). "Chromospheric activity catalogue of 4454 cool stars. Questioning the active branch of stellar activity cycles". Astronomy and Astrophysics 616: 616. doi:10.1051/0004-6361/201629518. Bibcode: 2018A&A...616A.108B.
- ↑ 7.0 7.1 7.2 Maldonado, J.; Micela, G.; Baratella, M.; d'Orazi, V.; Affer, L.; Biazzo, K.; Lanza, A. F.; Maggio, A. et al. (2020). "HADES RV programme with HARPS-N at TNG. XII. The abundance signature of M dwarf stars with planets". Astronomy and Astrophysics 644: A68. doi:10.1051/0004-6361/202039478. Bibcode: 2020A&A...644A..68M.
- ↑ Hojjatpanah, S.; Figueira, P.; Santos, N. C.; Adibekyan, V.; Sousa, S. G.; Delgado-Mena, E.; Alibert, Y.; Cristiani, S. et al. (2019). "Catalog for the ESPRESSO blind radial velocity exoplanet survey". Astronomy and Astrophysics 629: A80. doi:10.1051/0004-6361/201834729. Bibcode: 2019A&A...629A..80H.
- ↑ 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. doi:10.1051/0004-6361/202140985. Bibcode: 2021A&A...650A.201R. Data available at https://gruze.org/10pc/
- ↑ 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. doi:10.1093/mnras/stu358. Bibcode: 2014MNRAS.441.1545T.
- ↑ "The Habitable Exoplanets Catalog". University of Puerto Rico at Arecibo. http://phl.upr.edu/projects/habitable-exoplanets-catalog.
- ↑ Feng, Fabo; Butler, R. Paul; Shectman, Stephen A.; Crane, Jeffrey D.; Vogt, Steve; Chambers, John; Jones, Hugh R. A.; Wang, Sharon Xuesong et al. (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. doi:10.3847/1538-4365/ab5e7c. Bibcode: 2020ApJS..246...11F.
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