GJ 1002

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GJ 1002
GJ1002LightCurve.png
A light curve for GJ 1002, plotted from TESS data [1]
Observation data
Epoch J2000        Equinox J2000
Constellation Cetus [2]
Right ascension 00h 06m 43.19732s [3]
Declination −07° 32′ 17.0191″ [3]
Apparent magnitude  (V)13.837±0.003 [4]
Characteristics
Evolutionary stage Main sequence
Spectral type M5.5V [4]
Apparent magnitude  (V)13.837±0.003 [4]
Apparent magnitude  (G)11.774±0.003 [3]
Apparent magnitude  (J)8.323±0.019 [4]
Apparent magnitude  (H)7.792±0.034 [5]
Apparent magnitude  (K)7.439±0.021 [5]
Astrometry
Radial velocity (Rv)−40.46±0.30 [3] km/s
Proper motion (μ)RA: −811.566 mas/yr [3]
Dec.: −1893.251 mas/yr [3]
Parallax (π)206.3500±0.0474  mas [3]
Distance 15.806 ± 0.004  ly
(4.846 ± 0.001  pc)
Details [4]
Mass 0.120±0.010  M☉
Radius 0.137±0.005  R☉
Luminosity (bolometric)0.001406±0.000019  L☉
Surface gravity (log g)5.10±0.06  cgs
Temperature 3024±52  K
Metallicity [Fe/H]−0.25±0.19  dex
Rotation 161.28±2.93 [6] days
Other designations
NSV 15022, GJ 1002, G 158-27, LHS 2, NLTT 248, PLX 9.01, PM 00042-0747, TIC 176287658, 2MASS J00064325-0732147 [5]
Database references
SIMBAD data
Exoplanet Archive data

GJ 1002, or LHS 2, is a nearby red dwarf star, located 15.8 light-years (4.8 parsecs ) away from the Solar System in the constellation of Cetus. At an apparent magnitude of 13.8, it is much too faint to be visible to the naked eye. It hosts a system of two known exoplanets.

Contents

With a spectral type of M5.5V, this star is a red dwarf similar to Proxima Centauri. It has 12% the mass and 14% the radius of the Sun, and a temperature of 3,024  K (2,751  °C ; 4,984  °F ). [4] It is a slowly rotating star with a low level of magnetic activity. [7] Prior to the discovery of planets, it was an object of interest for the study of molecular features in its spectrum. [7] [8]

Planetary system

Two planetary companions to GJ 1002 were discovered in 2022 via radial velocity. Both have minimum masses close to that of Earth and orbit within the habitable zone of their star. While these planets do not transit their host star, it may be possible to determine the presence and composition of atmospheres with future instruments such as the ANDES spectrograph for the Extremely Large Telescope. [4]

As of 2023, GJ 1002 b & c are the fourth- and fifth-closest known Earth-mass exoplanets within the conservatively defined habitable zone, after Proxima Centauri b, GJ 1061 d, and Teegarden's Star c, and followed by Wolf 1069 b. [9]

The GJ 1002 planetary system [4]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b ≥1.08±0.13  M🜨 0.0457±0.001310.3465±0.027———
c≥1.36±0.17  M🜨 0.0738±0.002121.202±0.013———

See also

References

  1. ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 28 May 2023.
  2. ↑ Roman, Nancy G. (1987). "Identification of a constellation from a position". Publications of the Astronomical Society of the Pacific . 99 (617): 695. Bibcode:1987PASP...99..695R. doi: 10.1086/132034 . Constellation record for this object at VizieR.
  3. 1 2 3 4 5 6 7 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.
  4. 1 2 3 4 5 6 7 8 Suárez Mascareño, A.; González-Alvarez, E.; et al. (December 2022). "Two temperate Earth-mass planets orbiting the nearby star GJ 1002". Astronomy & Astrophysics . 670: A5. arXiv: 2212.07332 . Bibcode:2023A&A...670A...5S. doi:10.1051/0004-6361/202244991. S2CID   254353639.
  5. 1 2 3 "GJ 1002". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 28 November 2022.
  6. ↑ Kemmer, J.; Lafarga, M.; Fuhrmeister, B.; Shan, Y.; Schöfer, P.; Jeffers, S. V.; Caballero, J. A.; Quirrenbach, A.; Amado, P. J. (2025-04-11). "The CARMENES search for exoplanets around M dwarfs. Cluster analysis of signals from spectral activity indicators to search for shared periods". Astronomy and Astrophysics. 697. arXiv: 2504.08363 . Bibcode:2025A&A...697A.225K. doi:10.1051/0004-6361/202347056.
  7. 1 2 Wende, S.; Reiners, A.; Seifahrt, A.; Bernath, P. F. (November 2010). "CRIRES spectroscopy and empirical line-by-line identification of FeH molecular absorption in an M dwarf". Astronomy and Astrophysics . 523: A58. arXiv: 1007.4116 . Bibcode:2010A&A...523A..58W. doi:10.1051/0004-6361/201015220.
  8. ↑ Serindag, Dilovan B.; Snellen, Ignas A. G.; Mollière, Paul (November 2021). "Measuring titanium isotope ratios in exoplanet atmospheres". Astronomy & Astrophysics . 655: A69. arXiv: 2110.01908 . Bibcode:2021A&A...655A..69S. doi:10.1051/0004-6361/202141941.
  9. ↑ Kossakowski, D.; Kürster, M.; et al. (January 2023). "The CARMENES search for exoplanets around M dwarfs, Wolf 1069 b: Earth-mass planet in the habitable zone of a nearby, very low-mass star". Astronomy & Astrophysics . 670: A84. arXiv: 2301.02477 . Bibcode:2023A&A...670A..84K. doi:10.1051/0004-6361/202245322.
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