Gliese 1061 is a red dwarf star located approximately 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.
Location of Gliese 1061 in the constellation Horologium
The proper motion of Gliese 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.[7] The star displays no significant infrared excess due to circumstellar dust.[10]
Planetary system
On August 13, 2019, a planetary system was announced orbiting the star Gliese 1061 by the Red Dots project of detecting terrestrial planets around nearby red dwarf stars.[9] The planet Gliese 1061 d orbits in the conservative circumstellar habitable zone of its star and the planet Gliese 1061 c orbits in the inner edge of the habitable zone.[9] Gliese 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.[11]
Gliese 1061 c (also known as GJ 1061 c) is a potentially habitable exoplanet orbiting within the limits of the optimistic defined habitable zone of its red dwarf parent star.[12][13][9]
Gliese 1061 c is 75% more massive than the Earth.
The planet receives 35% more stellar flux than Earth and has an equilibrium temperature of 275K (2°C; 35°F).[14] The average temperature on the surface would be warmer, 34°C (307K; 93°F), provided the atmosphere is of similar composition to the Earth's.
Gliese 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.
Gliese 1061 d (also known as GJ 1061 d) is a potentially habitable exoplanet largely orbiting within the limits of the conservative defined habitable zone of its parent red dwarf star.[12][16][9]
The exoplanet is 68% more massive than the Earth.
The planet receives about 40% less stellar flux than Earth and has an estimated equilibrium temperature of 218K (−55°C; −67°F).[12][9] The average temperature on the surface would be colder than Earth's and at around 250K (−23°C; −10°F), provided the atmosphere is similar to that of Earth.
Gliese 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.[15] 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.[17]
Taking the absolute visual magnitude of Gliese 1061, , and the absolute visual magnitude of the Sun, , the visual luminosity of Gliese 1061 can therefore be calculated:
References
Cutri, R. M.; etal. (June 2003). "2MASS All-Sky Catalog of Point Sources". VizieR On-line Data Catalog: II/246. Bibcode:2003yCat.2246....0C.
"LHS 1565". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2008-12-11.
Scholz, R.-D.; etal. (2000). "New high-proper motion survey in the Southern sky". Astronomy and Astrophysics. 353: 958–969. Bibcode:2000A&A...353..958S.
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. S2CID235435757. 40.
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. arXiv:1908.04717. doi:10.1093/mnras/staa248. S2CID199551874.
Avenhaus, H.; etal. (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. S2CID56397054. A105.
Auclair-Desrotour, P.; etal. (2019). "Final spin states of eccentric ocean planets". Astronomy & Astrophysics. EDP Sciences. 629: A132. doi:10.1051/0004-6361/201935905. ISSN0004-6361. 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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