Gliese 832
  Gliese 832 Location of Gliese 832 in the constellationGrus | |
| Observation data EpochJ2000.0EquinoxJ2000.0 | |
|---|---|
| Constellation | Grus |
| Right ascension | 21h33m33.97512s[1] |
| Declination | −49° 00′ 32.3994″[1] |
| Apparent magnitude(V) | 8.66[2] |
| Characteristics | |
| Evolutionary stage | main-sequence star |
| Spectral type | M2V[3] |
| B−Vcolor index | 1.52[2] |
| Astrometry | |
| Radial velocity(Rv) | 12.72±0.13[1]km/s |
| Proper motion(μ) | RA:−45.917mas/yr[1] Dec.:−816.875mas/yr[1] |
| Parallax(π) | 201.3252 ± 0.0237mas[1] |
| Distance | 16.200 ± 0.002ly (4.9671 ± 0.0006pc) |
| Absolute magnitude(MV) | 10.19[2] |
| Details | |
| Mass | 0.441 ± 0.011[4]M☉ |
| Radius | 0.442 ± 0.018[4]R☉ |
| Luminosity (bolometric) | 0.0276 ± 0.0009[4]L☉ |
| Luminosity (visual, LV) | 0.007[note 1]L☉ |
| Surface gravity(logg) | 4.7[2]cgs |
| Temperature | 3,539+79 −74[4]K |
| Metallicity[Fe/H] | −0.06 ± 0.04[5]dex |
| Rotation | 37.5+1.4 −1.5d[6] |
| Age | 6±1.5[6]Gyr |
| Other designations | |
| Database references | |
| SIMBAD | The star |
| planet c | |
| planet b | |
| Exoplanet Archive | data |
| Data sources: | |
| Hipparcos Catalogue, HD | |
Gliese 832(Gl 832orGJ 832) is ared dwarfofspectral typeM2V in the southernconstellationGrus.[8]Theapparent visual magnitudeof 8.66[2]means that it is too faint to be seen with the naked eye. It is located relatively close to theSun,at a distance of 16.2light years[1]and has a highproper motionof 818.16 milliarcseconds per year.[1]Gliese 832 has just under half the mass and radius of the Sun.[8]Its estimated rotation period is a relatively leisurely 46 days.[3]The star is roughly 6 billion years old.[6]
This star achievedperihelionsome 52,920 years ago when it came within an estimated 15.71 ly (4.817 pc) of the Sun.[9]
Gliese 832 emits X-rays.[10]Despite the strongflare activity,Gliese 832 is producing on average less ionizing radiation than the Sun. Only at extremely short radiation wavelengths (<50nm) does its radiation intensity rise above the level of quiet Sun, but does not reach levels typical for active Sun.[11]
Planetary system
[edit]Gliese 832 hosts one known planet, with a second planet having been refuted in 2022.[6]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (years) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | 0.8+0.12 −0.11MJ |
3.53+0.15 −0.16 |
9.88+0.34 −0.33 |
0.069+0.026 −0.027 |
54.9+6.6 −4.9or125.1+4.9 −6.6° |
— |
Gliese 832 b
[edit]In September 2008, it was announced that aJupiter-like planet, designatedGliese 832 b,had been detected in a long-period, near-circular orbit around this star, with a false alarm probability of a negligible 0.05%. It would induce anastrometricperturbation on its star of at least 0.95milliarcsecondsand is thus a good candidate for being detected by astrometric observations. Despite its relatively large angular distance, direct imaging is problematic due to the star–planet contrast.[2]The orbital solution of the planet was refined in 2011.[13]In 2023, an astrometric detection of the planet was announced, determining its inclination and revealing atrue mass80% the mass of Jupiter.[12]
Gliese 832 c
[edit]Gliese 832 c was believed to be ofsuper-Earthmass.[8]It was announced to orbit in the optimistichabitable zonebut outside the conservative habitable zone of its parent star.[14]The planet Gliese 832 c was believed to be in, or very close to, the right distance from its sun to allow liquid water to exist on its surface.[8]However, doubts were raised about the existence of planet c by a 2015 study, which found that its orbital period is close to the stellar rotation period.[3]The existence of the planet was refuted in 2022, when a study found that theradial velocitysignal shows characteristics of a signal originating from stellar activity, and not from a planet.[6]
The region between Gliese 832 b and where Gliese 832 c would be is a zone where additional planets are possible.[15]
Search for cometary disc
[edit]If this system has a comet disc, it is not "brighter than the fractional dust luminosity 10−5"according to a 2012Herschelstudy.[16]
See also
[edit]Notes
[edit]- ^Using the absolute visual magnitude of Gliese 832and the absolute visual magnitude of the Sun,the visual luminosity can be calculated by
References
[edit]- ^abcdefgVallenari, A.; et al. (Gaia collaboration) (2023)."GaiaData 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.S2CID244398875. Gaia DR3 record for this sourceatVizieR.
- ^abcdef Bailey, J.; Butler, R. P.; Tinney, C. G.; Jones, H. R. A.; O'Toole, S.; Carter, B. D.; Marcy, G. W. (2009). "A Jupiter-like Planet Orbiting the Nearby M Dwarf GJ832".The Astrophysical Journal.690(1): 743–747.arXiv:0809.0172.Bibcode:2009ApJ...690..743B.doi:10.1088/0004-637X/690/1/743.S2CID17172233.
- ^abcSuárez Mascareño, A.; et al. (September 2015), "Rotation periods of late-type dwarf stars from time series high-resolution spectroscopy of chromospheric indicators",Monthly Notices of the Royal Astronomical Society,452(3): 2745–2756,arXiv:1506.08039,Bibcode:2015MNRAS.452.2745S,doi:10.1093/mnras/stv1441,S2CID119181646.
- ^abcdPineda, 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.S2CID235435757.40.
- ^Lindgren, Sara; Heiter, Ulrike (2017)."Metallicity determination of M dwarfs. Expanded parameter range in metallicity and effective temperature".Astronomy and Astrophysics.604:A97.arXiv:1705.08785.Bibcode:2017A&A...604A..97L.doi:10.1051/0004-6361/201730715.S2CID119216828.Archivedfrom the original on 2021-01-23.Retrieved2018-09-03.
- ^abcdeGorrini, P.; Astudillo-Defru, N.; et al. (August 2022). "Detailed stellar activity analysis and modelling of GJ 832: Reassessment of the putative habitable zone planet GJ 832c".Astronomy & Astrophysics.664:A64.arXiv:2206.07552.Bibcode:2022A&A...664A..64G.doi:10.1051/0004-6361/202243063.S2CID249674385.
- ^"Gliese 832".SIMBAD.Centre de données astronomiques de Strasbourg.Retrieved2018-09-23.
- ^abcd"Nearby Alien Planet May Be Capable of Supporting Life", Mike Wall, Space, June 25, 2014,http:// space /26357-exoplanet-habitable-zone-gliese-832c.htmlArchived2018-07-12 at theWayback Machine
- ^Bailer-Jones, C. A. L. (March 2015), "Close encounters of the stellar kind",Astronomy & Astrophysics,575:13,arXiv:1412.3648,Bibcode:2015A&A...575A..35B,doi:10.1051/0004-6361/201425221,S2CID59039482,A35.
- ^ Schmitt, J. H. M. M.; Fleming, T. A.; Giampapa, M. S. (1995)."The X-ray view of the low-mass stars in the solar neighborhood".The Astrophysical Journal.450(9): 392–400.Bibcode:1995ApJ...450..392S.doi:10.1086/176149.
- ^Fontenla, J. M.; Linsky, Jeffrey L.; Garrison, Jesse; France, Kevin; Buccino, A.; Mauas, Pablo; Vietes, Mariela; Walkowicz, Lucianne M. (2016)."Semi-Empirical Modeling of the Photosphere, Chromopshere, Transition Region, and Corona of the M-Dwarf Host Star Gj 832".The Astrophysical Journal.830(2): 154.arXiv:1608.00934.Bibcode:2016ApJ...830..154F.doi:10.3847/0004-637X/830/2/154.hdl:11336/21732.S2CID119279568.
- ^abXiao, Guang-Yao; Liu, Yu-Juan; et al. (March 2023). "The Masses of a Sample of Radial-Velocity Exoplanets with Astrometric Measurements".Research in Astronomy and Astrophysics.23(5).arXiv:2303.12409.Bibcode:2023RAA....23e5022X.doi:10.1088/1674-4527/accb7e.S2CID257663647.
- ^Bonfils, Xavier; Delfosse, Xavier; Udry, Stéphane; Forveille, Thierry; Mayor, Michel; Perrier, Christian; Bouchy, François; Gillon, Michaël; Lovis, Christophe; Pepe, Francesco; Queloz, Didier; Santos, Nuno C.; Ségransan, Damien; Bertaux, Jean-Loup (2011). "The HARPS search for southern extra-solar planets XXXI. The M-dwarf sample".Astronomy and Astrophysics.549:A109.arXiv:1111.5019.Bibcode:2013A&A...549A.109B.doi:10.1051/0004-6361/201014704.S2CID119288366.
- ^ Wittenmyer, R.A.; Tuomi, M.; Butler, R.P.; Jones, H. R. A.; O'Anglada-Escude, G.; Horner, J.; Tinney, C.G.; Marshall, J.P.; Carter, B.D.; et al. (2014). "GJ 832c: A super-earth in the habitable zone".The Astrophysical Journal.1406(2): 5587.arXiv:1406.5587.Bibcode:2014ApJ...791..114W.doi:10.1088/0004-637X/791/2/114.S2CID12157837.
- ^Satyal, S.; Griffith, J.; Musielak, Z. E. (2016), "Dynamics of a Probable Earth-mass Planet in GJ 832 System",The Astrophysical Journal,845(2): 106,arXiv:1604.04544,doi:10.3847/1538-4357/aa80e2,S2CID118663957
- ^ B. C. Matthews; forthcoming study promised inLestrade, J.-F.; Matthews, B. C.; Sibthorpe, B.; Kennedy, G. M.; Wyatt, M. C.; Bryden, G.; Greaves, J. S.; Thilliez, E.; Moro-Martín, A.; Booth, M.; Dent, W. R. F.; Duchêne, G.; Harvey, P. M.; Horner, J.; Kalas, P.; Kavelaars, J. J.; Phillips, N. M.; Rodriguez, D. R.; Su, K. Y. L.; Wilner, D. J. (2012). "A DEBRIS Disk Around The Planet Hosting M-star GJ581 Spatially Resolved with Herschel".Astronomy and Astrophysics.548:A86.arXiv:1211.4898.Bibcode:2012A&A...548A..86L.doi:10.1051/0004-6361/201220325.S2CID53704989.
