GJ 1061

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GJ 1061
Horologium constellation map.svg
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GJ 1061
Location of GJ 1061 in the constellation Horologium

Observation data
Epoch J2000       Equinox J2000
Constellation Horologium
Right ascension 03h 35m 59.69916s [1]
Declination −44° 30′ 45.7308″ [1]
Apparent magnitude  (V)13.03 [2]
Characteristics
Spectral type M5.5 V [2]
Apparent magnitude  (J)7.52 ± 0.02 [3]
U−B color index 1.52 [3]
B−V color index 1.90 [3]
Astrometry
Radial velocity (Rv)1.49±0.23 [1]  km/s
Proper motion (μ)RA: 745.654  mas/yr [1]
Dec.: −373.323  mas/yr [1]
Parallax (π)272.1615 ± 0.0316  mas [1]
Distance 11.984 ± 0.001  ly
(3.6743 ± 0.0004  pc)
Absolute magnitude  (MV)15.26 [4]
Details
Mass 0.125±0.003 [5]   M☉
Radius 0.152±0.007 [5]   R☉
Luminosity (bolometric)0.001641±0.000037 [5]   L☉
Luminosity (visual, LV)0.00007 [nb 1]   L☉
Temperature 2,977+72
−69 [5]   K
Metallicity [Fe/H]−0.03±0.09 [5]   dex
Rotational velocity (v sin i)≤ 5 [6]  km/s
Age >7.0±0.5 [7]   Gyr
Other designations
GJ 1061, LHS 1565, LFT 295, LTT 1702, LP 995-46, L 372-58 [3]
Database references
SIMBAD data
Exoplanet Archive data

GJ 1061 is a red dwarf star located 12 light-years (3.7 parsecs ) 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, [2] so it can only be seen with at least a moderately-sized telescope.

Contents

The proper motion of GJ 1061 has been known since 1974, but it was estimated to be further away: approximately 25 light-years (7.7 parsecs) distant based upon an estimated parallax of 0.130″. The RECONS accurately determined its distance in 1997. At that time, it was the 20th-nearest star system to the Sun. The discovery team noted that many more stars like this are likely to be discovered nearby. [2]

This star is a tiny, dim, red dwarf, close to the lower mass limit. It has an estimated mass of about 12.5% that of the Sun and is only about 0.2% as luminous. [5] The star displays no significant infrared excess due to circumstellar dust. [8]

Planetary system

On August 13, 2019, a planetary system was announced orbiting the star GJ 1061 by the Red Dots project for detecting terrestrial planets around nearby red dwarf stars. [7] The planet GJ 1061 d orbits in the conservative circumstellar habitable zone of its star and the planet GJ 1061 c orbits in the inner edge of the habitable zone. [7] GJ 1061 is a non-variable star that does not suffer flares, so there is a greater probability that the exoplanets still conserve their atmosphere if they had one. [9]

The GJ 1061 planetary system [7]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b ≥1.37+0.16
−0.15  M🜨 		0.021±0.0013.204±0.001<0.31——
c ≥1.74±0.23  M🜨 0.035±0.0016.689±0.005<0.29——
d ≥1.64+0.24
−0.23  M🜨 		0.054±0.00113.031+0.025
−0.032		<0.53——

GJ 1061 c

GJ 1061 c is a potentially habitable exoplanet orbiting within the limits of the optimistically defined habitable zone of its red dwarf parent star. [10] [11] [7]

GJ 1061 c is at least 74% more massive than the Earth. The planet receives 35% more stellar flux than Earth and has an equilibrium temperature of 275 K (2 °C; 35 °F). [12] The average temperature on the surface would be warmer, 34 °C (307 K; 93 °F), provided the atmosphere is of similar composition to the Earth's.

GJ 1061 c orbits its parent star very closely, every 6.7 days at a distance of just 0.035 au, so it is probably gravitationally locked and in synchronous rotation with its star.

GJ 1061 d

GJ 1061 d is a potentially habitable exoplanet largely orbiting within the limits of the conservatively defined habitable zone of its parent red dwarf star. [10] [13] [7]

The exoplanet is at least 64% more massive than the Earth. The planet receives about 40% less stellar flux than Earth and has an estimated equilibrium temperature of 218 K (−55 °C; −67 °F). [10] [7] The average temperature on the surface would be colder than Earth's and at around 250 K (−23 °C; −10 °F), provided the atmosphere is similar to that of Earth.

GJ 1061 d orbits its star every 13 days, and due to its close-in semi-major axis, it is likely that the exoplanet is tidally locked. [14] However, if the planet's orbit is confirmed to be highly eccentric then this eccentricity could be desynchronising it, enabling the existence of non-synchronised states of equilibrium in its rotation, relative to which side of the planet is facing the star, and thereby it will experience a day/night cycle. [15]

Another solution for this planet gives it a slightly shorter period of 12.4 days and a slightly smaller minimum mass of 1.53 ME. [7]

See also

Notes

  1. ↑ Taking the absolute visual magnitude of GJ 1061, , and the absolute visual magnitude of the Sun, , the visual luminosity of GJ 1061 can therefore be calculated:

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References

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  2. 1 2 3 4 Henry, Todd J.; et al. (1997). "The solar neighborhood IV: discovery of the twentieth nearest star". The Astronomical Journal . 114: 388–395. Bibcode:1997AJ....114..388H. doi:10.1086/118482.
  3. 1 2 3 4 "LHS 1565". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2008-12-11.
  4. ↑ Scholz, R.-D.; et al. (2000). "New high-proper motion survey in the Southern sky". Astronomy and Astrophysics . 353: 958–969. Bibcode:2000A&A...353..958S.
  5. 1 2 3 4 5 6 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.
  6. ↑ Barnes, J. R.; et al. (April 2014). "Precision radial velocities of 15 M5-M9 dwarfs". Monthly Notices of the Royal Astronomical Society . 439 (3): 3094–3113. arXiv: 1401.5350 . Bibcode:2014MNRAS.439.3094B. doi: 10.1093/mnras/stu172 . S2CID   16005221.
  7. 1 2 3 4 5 6 7 8 Dreizler, S.; Jeffers, S. V.; Rodríguez, E.; Zechmeister, M.; Barnes, J.R.; Haswell, C.A.; Coleman, G. A. L.; Lalitha, S.; Hidalgo Soto, D.; Strachan, J.B.P.; Hambsch, F-J.; López-González, M. J.; Morales, N.; Rodríguez López, C.; Berdiñas, Z. M.; Ribas, I.; Pallé, E.; Reiners, Ansgar; Anglada-Escudé, G. (2019-08-13). "Red Dots: A temperate 1.5 Earth-mass planet in a compact multi-terrestrial planet system around GJ1061". Monthly Notices of the Royal Astronomical Society . 493 (1): 536. arXiv: 1908.04717 . Bibcode:2020MNRAS.493..536D. doi: 10.1093/mnras/staa248 . S2CID   199551874.
  8. ↑ Avenhaus, H.; et al. (December 2012). "The nearby population of M-dwarfs with WISE: a search for warm circumstellar dust". Astronomy & Astrophysics . 548: 15. arXiv: 1209.0678 . Bibcode:2012A&A...548A.105A. doi:10.1051/0004-6361/201219783. S2CID   56397054. A105.
  9. ↑ Starr, Michelle (27 August 2019). "Three Rocky Exoplanets Have Been Found Orbiting a Star Just 12 Light-Years Away". ScienceAlert. Retrieved 2020-10-07.
  10. 1 2 3 "The Habitable Exoplanets Catalog - Planetary Habitability Laboratory @ UPR Arecibo". phl.upr.edu. Retrieved 2020-03-31.
  11. ↑ "Exoplanet-catalog". Exoplanet Exploration: Planets Beyond our Solar System. Retrieved 2020-03-31.
  12. ↑ "Trio of Super-Earths Found Orbiting Red Dwarf Gliese 1061 | Astronomy | Sci-News.com". Breaking Science News | Sci-News.com. Retrieved 2020-03-31.
  13. ↑ "GJ 1061 d". exoplanetarchive.ipac.caltech.edu. Retrieved 2020-10-07.
  14. ↑ "Exoplanet-catalog". Exoplanet Exploration: Planets Beyond our Solar System. Retrieved 2020-10-07.
  15. ↑ Auclair-Desrotour, P.; et al. (2019). "Final spin states of eccentric ocean planets". Astronomy & Astrophysics. 629. EDP Sciences: A132. arXiv: 1907.06451 . Bibcode:2019A&A...629A.132A. doi: 10.1051/0004-6361/201935905 . ISSN   0004-6361. While the semidiurnal tide drives the body towards the spin-orbit synchronous rotation, eccentricity tides tend to desynchronise it, and thereby enable the existence of non-synchronised states of equilibrium.
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