Gliese 832

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Gliese 832
Grus constellation map.svg
Red pog.png
Gliese 832
Location of Gliese 832 in the constellation Grus

Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Grus
Right ascension 21h 33m 33.97512s [1]
Declination −49° 00′ 32.3994″ [1]
Apparent magnitude  (V)8.66 [2]
Characteristics
Evolutionary stage main-sequence star
Spectral type M2V [3]
B−V color index 1.52 [2]
Astrometry
Radial velocity (Rv)12.72±0.13 [1]  km/s
Proper motion (μ)RA: −45.917  mas/yr [1]
Dec.: −816.875  mas/yr [1]
Parallax (π)201.3252 ± 0.0237  mas [1]
Distance 16.200 ± 0.002  ly
(4.9671 ± 0.0006  pc)
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 (log g)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
−1.5 d [6]
Age 6±1.5 [6]   Gyr
Other designations
CD−49°13515, GJ  832, HD  204961, HIP  106440, L  354-89, LHS  3685, PLX  5190, TIC  139754153, TYC  8431-60-1, 2MASS J21333397-4900323 [7]
Database references
SIMBAD The star
planet c
planet b
Exoplanet Archive data
Extrasolar Planets
Encyclopaedia 		data
Data sources:
Hipparcos Catalogue,
HD

Gliese 832 (Gl 832 or GJ 832) is a red dwarf of spectral type M2V in the southern constellation Grus. [8] The apparent visual magnitude of 8.66 [2] 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 [1] and has a high proper motion of 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]

Contents

This star achieved perihelion some 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 strong flare 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

Gliese 832 hosts one known planet, with a second planet having been refuted in 2022. [6]

The Gliese 832 planetary system [12]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(years)		 Eccentricity Inclination Radius
b 0.8+0.12
−0.11  MJ 		3.53+0.15
−0.16		9.88+0.34
−0.33		0.069+0.026
−0.027		54.9+6.6
−4.9 or 125.1+4.9
−6.6 ° 		—

Gliese 832 b

In September 2008, it was announced that a Jupiter-like planet, designated Gliese 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 an astrometric perturbation on its star of at least 0.95 milliarcseconds and 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 a true mass 80% the mass of Jupiter. [12]

Gliese 832 c

Gliese 832 c was believed to be of super-Earth mass. [8] It was announced to orbit in the optimistic habitable zone but 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 the radial velocity signal 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

If this system has a comet disc, it is not "brighter than the fractional dust luminosity 10−5" according to a 2012 Herschel study. [16]

See also

Notes

  1. ↑ Using the absolute visual magnitude of Gliese 832 and the absolute visual magnitude of the Sun , the visual luminosity can be calculated by

Related Research Articles

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Gliese 832 b is a gas giant exoplanet about 80% the mass of Jupiter, located 16.2 light-years from the Sun in the constellation of Grus, orbiting the red dwarf star Gliese 832.

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GJ 625 is a small red dwarf star with an exoplanetary companion in the northern constellation of Draco. The system is located at a distance of 21.1 light-years from the Sun based on parallax, but is drifting closer with a radial velocity of −13 km/s. It is too faint to be visible to the naked eye, having an apparent visual magnitude of 10.13 and an absolute magnitude of 11.06.

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References

  1. 1 2 3 4 5 6 7 8 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. 1 2 3 4 5 6 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. S2CID   17172233.
  3. 1 2 3 Suárez 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, S2CID   119181646.
  4. 1 2 3 4 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.
  5. ↑ 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. S2CID   119216828.
  6. 1 2 3 4 5 Gorrini, 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. S2CID   249674385.
  7. ↑ "Gliese 832". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2018-09-23.
  8. 1 2 3 4 "Nearby Alien Planet May Be Capable of Supporting Life", Mike Wall, Space.com, June 25, 2014, http://www.space.com/26357-exoplanet-habitable-zone-gliese-832c.html
  9. ↑ 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, S2CID   59039482, A35.
  10. ↑ 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 .
  11. ↑ 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. Bibcode:2016ApJ...830..154F. doi: 10.3847/0004-637X/830/2/154 . hdl: 11336/21732 . S2CID   119279568.
  12. 1 2 Xiao, 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. S2CID   257663647.
  13. ↑ 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. S2CID   119288366.
  14. ↑ 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. S2CID   12157837.
  15. ↑ 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 , S2CID   118663957
  16. ↑ B. C. Matthews; forthcoming study promised in Lestrade, 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. S2CID   53704989.
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