GJ 1061

The following article will address the topic of GJ 1061, which has been the subject of great interest for a long time. GJ 1061 is a topic that has generated debate in different areas and has aroused the curiosity of many. Throughout history, GJ 1061 has been the subject of study and research, which has led to significant discoveries and advances in the understanding of this topic. Through this article, different aspects related to GJ 1061 will be explored, delving into its importance, impact and possible implications in various contexts. In addition, different perspectives and approaches will be analyzed to better understand GJ 1061 and its implications today.

GJ 1061
GJ 1061 is located in the constellation Horologium.
GJ 1061 is located in the constellation Horologium.
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[4]
B−V color index 1.90[4]
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]
Distance11.984 ± 0.001 ly
(3.6743 ± 0.0004 pc)
Absolute magnitude (MV)15.26[5]
Details
Mass0.125±0.003[6] M☉
Radius0.152±0.007[6] R☉
Luminosity (bolometric)0.001641±0.000037[6] L☉
Luminosity (visual, LV)0.00007[a] L☉
Temperature2,977+72
−69[6] K
Metallicity −0.03±0.09[6] dex
Rotation~125 d[3]
Rotational velocity (v sin i)<2.5[3] km/s
Age>7.0±0.5[7] Gyr
Other designations
GJ 1061, L 372-58, LFT 295, LHS 1565, LP 995-46, LTT 1702[4]
Database references
SIMBADdata
Exoplanet Archivedata

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.

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.[6] It is an old, slowly-rotating star, with an age of at least 7 billion years and a rotation period of about 125 days.[3] The star displays no significant infrared excess due to circumstellar dust.[8] It hosts a system of three known exoplanets.[3]

History of observations

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 known star system to the Sun. The discovery team noted that many more stars like this are likely to be discovered nearby.[2]

Planetary system

On August 13, 2019, a system of three planets was announced orbiting the star GJ 1061 by the Red Dots project for detecting terrestrial planets around nearby red dwarf stars.[7] Since the planets were detected by the radial velocity method, initially only their minimum masses were known. Further observations allowed the true masses to be determined based on gravitational interactions between the planets.[b] All three planets are less than twice the mass of Earth, and so are likely to be rocky planets.[3]

The planet GJ 1061 d orbits in the conservative habitable zone of its star, and the planet GJ 1061 c orbits near the inner edge of the habitable zone.[7] As of 2025, they are the third- and fourth-nearest known terrestrial exoplanets in the habitable zone, after Proxima Centauri b and Ross 128 b.[3] GJ 1061 is a non-variable star that does not suffer flares, so there is a greater probability that the exoplanets still conserve their atmospheres if they had them.[9]

The GJ 1061 planetary system[3][c]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b 1.11+0.11
−0.09 M🜨 		0.0210±0.0006 3.2073+0.0002
−0.0003 		0.05+0.5
−0.03 		~77° —
c 1.81+0.13
−0.11 M🜨 		0.0342+0.0009
−0.0010 		6.6821±0.0008 0.02+0.03
−0.02 		~77° —
d 1.67+0.17
−0.16 M🜨 		0.054±0.002 13.066±0.002 0.04+0.04
−0.03 		~77° —

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 about 81% more massive than the Earth.[3] 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 tidally 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 about 67% more massive than the Earth.[3] 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:
  2. ^ This was previously done for the Gliese 876 and Gliese 581 systems.
  3. ^ Data taken from "coplanar, Model D5" solution in Table 4.

References

  1. ^ a b c d e 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. ^ a b c d 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. ^ a b c d e f g h i j Dreizler, S.; Jeffers, S. V.; et al. (April 2025). "RedDots: Planetary masses in the GJ1061 system from planet-planet interaction". Astronomy & Astrophysics. arXiv:2504.10926.
  4. ^ a b c "LHS 1565". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2008-12-11.
  5. ^ 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.
  6. ^ a b c d e f 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.
  7. ^ a b c d e f g 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. ^ a b c "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.