GJ 1132

Last updated
GJ 1132
Observation data
Epoch J2000       Equinox J2000
Constellation Vela
Right ascension 10h 14m 51.77869s [1]
Declination −47° 09′ 24.1928″ [1]
Apparent magnitude  (V)13.46 [2]
Characteristics
Evolutionary stage Main sequence
Spectral type M4 [2]
Astrometry
Radial velocity (Rv)34.66±0.48 [1]  km/s
Proper motion (μ)RA: −1,054.201  mas/yr [1]
Dec.: +414.512  mas/yr [1]
Parallax (π)79.3206 ± 0.0182  mas [1]
Distance 41.119 ± 0.009  ly
(12.607 ± 0.003  pc)
Details
Mass 0.194±0.005 [3]   M☉
Radius 0.215±0.009 [3]   R☉
Luminosity 0.00436±0.00013 [3]   L☉
Temperature 3,196±71 [3]   K
Rotation 122.3+6.0
−5.0 d [4]
Other designations
RAVE J101451.9-470925, Gaia DR2  5413438219396893568, GJ  1132, L  320-124, LFT  707, LHS  281, LTT  3758, NLTT  23819, PM  10129-4655, PM  J10148-4709, GCRV  26265, 2MASS J10145184-4709244, WISEA J101450.66-470919.7 [5]
Database references
SIMBAD data
Exoplanet Archive data

GJ 1132 is a small red dwarf star 41.1 light-years (12.6 parsecs ) away from Earth [1] in the constellation Vela. In 2015, it was revealed to have a hot rocky Earth-sized planet orbiting it every 1.6 days. [6] In 2018, a second planet and a potential third were revealed. [4]

Contents

Planetary system

As of June 12, 2018, there are two confirmed exoplanets and one candidate exoplanet orbiting GJ 1132.

GJ 1132 b

GJ 1132 b is the innermost planet of the GJ 1132 system, as well as the smallest. It is very similar in size and mass to Earth, with a radius of 1.13 R🜨 and a mass of 1.66 ME. It is slightly denser than Earth with 30% more surface gravity, meaning it has a rocky composition. [4] Despite its physical similarities to Earth, it is considered too hot to be habitable, getting 19 times more sunlight due to its 1.6 day orbital period. As of 2022, it remains unclear whether the planet has an atmosphere, with some studies finding evidence for an atmosphere, [7] [8] but others finding a flat, featureless spectrum that leaves the presence or absence of an atmosphere inconclusive. [9] [10] [11]

GJ 1132 c

GJ 1132 c was reported by Bonfils and colleagues using the HARPS spectrograph on the ESO 3.6 m Telescope at the La Silla Observatory in Chile in June 2018. No transits of the planet were found, but it has a minimum mass of about 2.6 ME and gets 1.9 times the amount of sunlight as Earth with an equilibrium temperature of 300 K (27 °C; 80 °F). It orbits outside the inner limit of GJ 1132's habitable zone (which ends at 1.6 times the stellar flux of Earth), but because the exact characteristics of the planet's atmosphere are unknown, it has been mentioned that it could still be potentially habitable. However, with a lack of transits, determining its atmospheric characteristics will be extremely difficult. [4]

GJ 1132 d

An unconfirmed cold super-Earth candidate was also detected, with a minimum mass of about 8.4 ME and a low equilibrium temperature of 111 K (−162 °C; −260 °F). It has been designated GJ 1132 (d) with parenthesis because it is not considered a confirmed planet. Despite the signal having a false alarm probability of less than 0.01%, comparable to GJ 1132 b and c, it is close to the period of the star's magnetic cycle. [4]

Artist's impression and size comparison of the two confirmed planets of GJ 1132 with Earth GJ 132bc.jpg
Artist's impression and size comparison of the two confirmed planets of GJ 1132 with Earth
The GJ 1132 planetary system [4] [12]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b 1.66 ± 0.23  M🜨 0.0153 ± 0.00051.6289304(13) [13] <0.2286.58 ± 0.63° 1.13 ± 0.056  R🜨
c>2.64 ± 0.44  M🜨 0.0476 ± 0.00178.929 ± 0.010<0.27——
d(unconfirmed)>8.4 +1.7
−2.5 M🜨 		0.35 ± 0.01176.9 ± 5.1<0.53——

See also

Related Research Articles

GJ 1061 is a red dwarf star located 12 light-years from Earth in the southern constellation of Horologium. Even though it is a relatively nearby star, it has an apparent visual magnitude of about 13, so it can only be seen with at least a moderately-sized telescope.

<span class="mw-page-title-main">HD 219134</span> Star in the constellation Cassiopeia

HD 219134 is a main-sequence star in the constellation of Cassiopeia. It is smaller and less luminous than the Sun, with a spectral class of K3V, which makes it an orange-hued star. HD 219134 is relatively close to our system, with an estimated distance of 21.34 light years. This star is close to the limit of apparent magnitude that can still be seen by the unaided eye. The limit is considered to be magnitude 6 for most observers. This star has a magnitude 9.4 optical companion at an angular separation of 106.6 arcseconds.

Gliese 180, is a small red dwarf star in the equatorial constellation of Eridanus. It is invisible to the naked eye with an apparent visual magnitude of 10.9. The star is located at a distance of 39 light years from the Sun based on parallax, and is drifting closer with a radial velocity of −14.6 km/s. It has a high proper motion, traversing the sky at the rate of 0.765 arcseconds per year.

<span class="mw-page-title-main">GJ 1132 b</span> Terrestrial exoplanet orbiting GJ 1132

GJ 1132 b is an exoplanet orbiting GJ 1132, a red dwarf star 41 light-years from Earth, in the constellation Vela. The planet is considered uninhabitable but cool enough to possess an atmosphere. GJ 1132 b was discovered by the MEarth-South array in Chile.

<span class="mw-page-title-main">LHS 1140</span> Star in the constellation Cetus

LHS 1140 is a red dwarf in the constellation of Cetus. Based on stellar parallax measurement, it is 48.8 light-years away from the Sun. 'LHS' refers to the Luyten Half-Second Catalogue of stars with proper motions exceeding half a second of arc annually. The star is over 5 billion years old and has only about 18% the mass of the Sun and 21% of its radius. LHS 1140's rotational period is 130 days. No flares have been observed.

GJ 9827 is a star in the constellation of Pisces. It is a K-type main-sequence star with an apparent magnitude of 10.250. It is 97 light-years away, based on parallax.

TOI-700 is a red dwarf 101.4 light-years away from Earth located in the Dorado constellation that hosts TOI-700 d, the first Earth-sized exoplanet in the habitable zone discovered by the Transiting Exoplanet Survey Satellite (TESS).

<span class="mw-page-title-main">LTT 1445</span> Star system in the constellation Eridanus

LTT 1445 is a triple M-dwarf system 22.4 light-years distant in the constellation Eridanus. The primary LTT 1445 A hosts two exoplanets—one discovered in 2019 that transits the star every 5.36 days, and another found in 2021 that transits the star every 3.12 days, close to a 12:7 resonance. As of October 2022 it is the second closest transiting exoplanet system discovered, with the closest being HD 219134 bc.

<span class="mw-page-title-main">Gliese 486</span> Star in constellation of Virgo

Gliese 486, also known as Wolf 437 and formally named Gar, is a red dwarf star 26.4 light-years away in the constellation Virgo. It hosts one known exoplanet.

L 98-59 is a bright M dwarf star, located in the constellation of Volans, at a distance of 10.608 parsecs, as measured by the Gaia spacecraft.

HD 106315, or K2-109, is a single star with a pair of close-orbiting exoplanets, located in the constellation of Virgo. Based on parallax measurements, this system lies at a distance of 356 light years from the Sun. At that range, the star is too faint to be seen with the naked eye, as it has an apparent visual magnitude of 8.95. But it is slowly drifting closer with a radial velocity of −3 km/s. As of 2020, multiplicity surveys have not detected any stellar companions to HD 106315.

<span class="mw-page-title-main">Wolf 1069</span> Red dwarf star in the constellation Cygnus

Wolf 1069 is a red dwarf star located 31.2 light-years away from the Solar System in the constellation of Cygnus. The star has 17% the mass and 18% the radius of the Sun, a temperature of 3,158 K, and a slow rotation period of 150–170 days. It hosts one known exoplanet called Wolf 1069 b which could possibly sustain life.

References

  1. 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.
  2. 1 2 Bidelman, W. P. (October 1985), "G. P. Kuiper's spectral classifications of proper-motion stars", The Astrophysical Journal Supplement Series, 59: 197–227, Bibcode:1985ApJS...59..197B, doi: 10.1086/191069 .
  3. 1 2 3 4 Pineda, J. Sebastian; et al. (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.
  4. 1 2 3 4 5 6 Bonfils, X.; et al. (October 2018), "Radial velocity follow-up of GJ1132 with HARPS. A precise mass for planet 'b' and the discovery of a second planet", Astronomy & Astrophysics, 618: 12, arXiv: 1806.03870 , Bibcode:2018A&A...618A.142B, doi:10.1051/0004-6361/201731884, S2CID   119394477, A142.
  5. ↑ "GJ 1132". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2020-08-31.
  6. ↑ Berta-Thompson, Zachory K.; et al. (2015). "A rocky planet transiting a nearby low-mass star". Nature. 527 (7577): 204–207. arXiv: 1511.03550 . Bibcode:2015Natur.527..204B. doi:10.1038/nature15762. PMID   26560298. S2CID   4385619.
  7. ↑ "Atmosphere around super-Earth detected", phys.org, April 6, 2017, retrieved April 6, 2017.
  8. ↑ Swain, Mark R.; Estrela, Raissa; Roudier, Gael M.; Sotin, Christophe; Rimmer, Paul B.; Valio, Adriana; West, Robert; Pearson, Kyle; Huber-Feely, Noah; Zellem, Robert T. (2021). "Detection of an Atmosphere on a Rocky Exoplanet". The Astronomical Journal. 161 (5): 213. arXiv: 2103.05657 . Bibcode:2021AJ....161..213S. doi: 10.3847/1538-3881/abe879 . S2CID   232170188.
  9. ↑ Diamond-Lowe, Hannah; et al. (2018). "Ground-based Optical Transmission Spectroscopy of the Small, Rocky Exoplanet GJ 1132b". The Astronomical Journal. 156 (2) 42. arXiv: 1805.07328 . Bibcode: 2018AJ....156...42D . doi: 10.3847/1538-3881/aac6dd . S2CID   119061941.
  10. ↑ Mugnai, Lorenzo V.; Modirrousta-Galian, Darius; Edwards, Billy; Changeat, Quentin; Bouwman, Jeroen; Morello, Giuseppe; Al-Refaie, Ahmed; Baeyens, Robin; Bieger, Michelle Fabienne; Blain, Doriann; Gressier, Amélie (2021-04-05). "ARES.* V. No Evidence for Molecular Absorption in the HST WFC3 Spectrum of GJ 1132 b". The Astronomical Journal. 161 (6): 284. arXiv: 2104.01873 . Bibcode:2021AJ....161..284M. doi: 10.3847/1538-3881/abf3c3 . S2CID   233025360.
  11. ↑ Libby-Roberts, Jessica E.; Berta-Thompson, Zachory K.; Diamond-Lowe, Hannah; Gully-Santiago, Michael A.; Irwin, Jonathan M.; Kempton, Eliza M.-R.; Rackham, Benjamin V.; Charbonneau, David; Desert, Jean-Michel; Dittmann, Jason A.; Hofmann, Ryan (2022). "The Featureless HST/WFC3 Transmission Spectrum of the Rocky Exoplanet GJ 1132b: No Evidence for a Cloud-free Primordial Atmosphere and Constraints on Starspot Contamination". The Astronomical Journal. 164 (2): 59. arXiv: 2105.10487 . Bibcode:2022AJ....164...59L. doi: 10.3847/1538-3881/ac75de . S2CID   235125875.
  12. ↑ "GJ 1132 b Confirmed Planet Overview Page", NASA Exoplanet Archive, retrieved 2018-06-11.
  13. ↑ Kokori, A.; et al. (14 February 2023). "ExoClock Project. III. 450 New Exoplanet Ephemerides from Ground and Space Observations". The Astrophysical Journal Supplement Series. 265 (1) 4. arXiv: 2209.09673 . Bibcode: 2023ApJS..265....4K . doi: 10.3847/1538-4365/ac9da4 . Vizier catalog entry
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.