Gliese 667 C

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Gliese 667 C
Diagram showing star positions and boundaries of the constellation of Scorpius and its surroundings
Cercle rouge 100%.svg

A star chart of the constellation of Scorpius showing the position of Gliese 667 (red circle at lower left)
Observation data
Epoch J2000      Equinox J2000
Constellation Scorpius
Right ascension 17h 18m 57.16483s[1]
Declination −34° 59′ 23.1416″[1]
Apparent magnitude (V) 10.20[2]
Spectral type M1.5V[2][3]
U−B color index 1.17
B−V color index 1.57
Variable type flare star
Radial velocity (Rv) 6.5[4] km/s
Proper motion (μ) RA: 1129.76[1] mas/yr
Dec.: −77.02[1] mas/yr
Parallax (π) 146.29 ± 9.03[1] mas
Distance 22 ± 1 ly
(6.8 ± 0.4 pc)
Absolute magnitude (MV) 11.03
Mass 0.31[4] M
Radius 0.42[2] R
Luminosity 0.0137[4] L
Temperature 3,700 ± 100[4] K
Metallicity [Fe/H] –0.59 ± 0.10[4] dex
Rotation 105 days [4]
Age 2-10[4] Gyr
Other designations
LHS 443, 142 G. Scorpii C, CD−34°11626C, GJ 667 C, HD 156384 C, HIP 84709 C, HR 6426 C, SAO 208670 C
Database references
Exoplanet Archive data
Extrasolar Planets

Gliese 667 C, also known as GJ 667 C, is a component of the Gliese 667 triple star system. Located 6.8 parsecs (22 light-years) away from the Solar System in the constellation Scorpius, Gliese 667 C is a red dwarf[5] with 1.4% of the luminosity of the Sun and a relatively cool effective temperature of 3,700 K at its surface.[4] It is the smallest and least massive member[2][6] of the Gliese 667 system. Gliese 667 C has been found to have a system of two confirmed extrasolar planets, all of which are sub-Neptunes or super-Earths detected using the radial velocity method.[7] The outer planet Gliese 667 Cc orbits within the habitable zone.[7] Additional planets have been proposed, including two that would be located in the habitable zone. These may artifacts caused by failing to account for correlated noise in the data.[8]

Stellar properties[edit]

Gliese 667 C is a class M2V star that orbits at a projected separation of 230 AU from Gliese 667 AB, and is believed to be at least two billion years old.[7]


Although M-class stars can remain active for much longer than the Sun, Gliese 667 C is now a relatively inactive star. This allowed investigation of its planetary system by examining small variations in its radial velocity. At the current time, it means that the planets would receive negligible levels of UV and X-ray radiation from chromospheric emission of the star and stellar flares.[7]

Habitable zone[edit]

The habitable zone of a star has been defined as a "Goldilocks region" of space which is neither too hot nor too cold for a planet with liquid water under an Earth-like atmosphere. The planet must be far enough away from its star to avoid a "moist greenhouse" in which water vapor retains so much heat that any ocean would boil and hydrogen would be lost to space, but close enough to avoid global ice coverage. The most recently published calculations of the habitable zone, when applied to the Gliese 667 C system, predict that the habitable zone extends from an inner edge around 0.095–0.126 AU to an outer edge of 0.241–0.251 AU. A broader definition of the zone might apply if planets with small but non-negligible amounts of water were detected.[7][9]

Planetary system[edit]

As of June 28, 2013, the most recent orbital solution proposes two certainly detected planet candidates (b and c). Additional planet candidates have been proposed (d, e, f, g, and h).[7] These may, however, be artifacts caused by failure to properly take correlated noise in the radial-velocity data into account.[8] Planet c is a sub-Neptune or super-Earth orbiting within the habitable zone of the star.[7][10] The naming of the planet candidates slightly changed with time. The current naming is based on the seven-planet solution released on June 2013.[7]

The Gliese 667 C system
(in order from star)
Mass Semimajor axis
Orbital period
Eccentricity Inclination Radius
b 5.94–12 M 0.050 432 ± 0.000 001 7.2006 0.112 >30°
h (unconfirmed) 1.1–2.2 M 0.085 ~17 >30°
c 3.86–7.8 M 0.125 07 ± 0.000 06 28.1231 0.001 >30°
f (unconfirmed) 1.94–4 M 0.155 75 ± 0.000 17 39.0819 0.001 >30°
e (unconfirmed) 2.68–5.4 M 0.212 57 ± 0.000 35 62.2657 0.001 >30°
d (unconfirmed) 5.21–10.4 M 0.275 8 ± 0.000 3 92.0926 0.019 >30°
g (unconfirmed) 4.41–8.8 M 0.538 9 ± 0.000 5 251.519 0.107 >30°

Early planetary solutions[edit]

This animation shows the orbital motions of the proposed planet candidates (white dots and ellipses) around Gliese 667C in the most recently proposed orbital solution with 7 planets.[7] Three of these planets are super-Earths mass objects orbiting in the habitable zone (shown in green) where widespread surface liquid water may exist. The orbit of the planet Mercury in the Solar System is included for scale, in blue. (File link)
This video shows an artist’s impression of the view from the exoplanet Gliese 667Cd looking towards the planet’s parent star (Gliese 667C). In the background to the right the more distant stars in this triple system (Gliese 667A and Gliese 667B) are visible and to the left in the sky one of the other planets, the newly discovered Gliese 667Ce, can be seen as a crescent. Gliese 667Cd itself is thought to be a cold planet, somewhat like Mars. (File link)
An artist's impression of GJ 667 Cc, a potentially habitable planet orbiting a red dwarf constituent in a ternary star system. (File link)

Gliese 667 Cb, the first planet of the system to be reported, was first announced by the European Southern Observatory's HARPS group on 19 October 2009, together with 29 other planets. Gliese 667 Cc was first mentioned in a pre-print made public on 21 November 2011, claiming that a discovery paper from the same group was in preparation.[11] However, the announcement of a refereed journal report came on 2 February 2012 by researchers at the Carnegie Institution for Science and the University of Göttingen.[4][12] In that announcement, Gliese 667 Cc was described as one of the best candidates yet found to harbor liquid water, and thus, potentially, support life on its surface.[13] A detailed orbital analysis and refined orbital parameters for Gliese 667 Cc were also presented at the time.[4]

Based on GJ 667 C's bolometric luminosity, GJ 667 Cc would receive 90% of the light Earth does;[14] however much of that electromagnetic radiation would be in the invisible infrared. Based on blackbody temperature calculations, GJ 667 Cc should absorb more overall electromagnetic radiation and thereby have an equilibrium temperature of 277.4 K, as compared with 254.3 K for the Earth.[4]

Preliminary radial-velocity measurements indicated the presence of an additional super-Earth candidate (Gliese 667 Cd), orbiting in an "extended habitable zone" where large quantities of CO2 and other greenhouse gases may make life possible (a planet similar to Gliese 581 d).[13] However, this candidate was less certain at the time due to similarities of the period to rather clear signals detected in several activity indices. Its phase sampling was also sparse, causing severe aliasing and potential confusion. Another likely period for this same candidate was proposed to be 91 days.[4] An additional, long-period signal was found in the data. While the trend is largely consistent with the star's orbit around the A/B primary, a minor curvature in the trend suggests that the object may have a shorter period. A preliminary solution of 7100 days was derived which consistent with a roughly Saturn-mass planet. Not enough data was available to decide conclusively the nature of such long-period trend.[4]

The Gliese 667 C: four-planet solution system[4]
(in order from star)
Mass Semimajor axis
Orbital period
Eccentricity Inclination Radius
b ≥5.68 ± 0.23 M 0.049 7.20066 ± 0.00067 0.172 ± 0.043
c ≥4.54 ± 0.38 M 0.123 ± 0.02 28.155 ± 0.017 <0.27
d (unconfirmed) ≥5.65 ± 0.54 M 0.235 74.79 ± 0.13 / 91 ± 0.5 0 (fixed)
(trend) ≥0.25 ± 0.12 MJ 2.577 7100 ± 3000 0 (fixed)

In December 2012, a new solution was obtained using HARPS data only. Such solution contained 6 Doppler signals that were tentatively associated to 5 to 6 planet candidates.[10] The 7.2 and 28.1 days signals correspond to the periods of two previously known planets around the star. Among the other signals, one was suspected to be generated by stellar activity and another one was proposed at a period of 30 days, too close to 28.1 days (period of the securely detected GJ 667Cc) to be in a stable orbit. In an informal interview, Guillem Anglada-Escudé, of the original discovery team, noted that the corresponding system of planets was unstable, and that the possibility of astrophysical false-positives had not been properly done to distinguish between activity induced and genuine Keplerian signals.[15] The claim appeared as a submitted article (not yet accepted by June 2013) and the proposed solution lacked of several basic checks. Therefore, the claim was considered preliminary but suggestive.

The Gliese 667 C: five-planet solution system[10]
(in order from star)
Mass Semimajor axis
Orbital period
Eccentricity Inclination Radius
b ≥5.4+0.3
c ≥4.8+0.5
d (unconfirmed) ≥3.1+0.4
e (unconfirmed) ≥2.4+0.4
f (unconfirmed) ≥5.4+0.5

The seven-planet solution[edit]

On 25 June 2013 a new orbital solution was announced by the initial discovery team, with five robustly detected planets and two less certain objects. Of the five secure planets, three—Gliese 667Cc, Cf, and Ce—would be located in the habitable zone of the star. Gliese 667 Cf has an orbital period of about 39 days, while Gliese 667 Ce has a longer orbital period of roughly 62 days (but a 53.2-day orbital period for this candidate is still possible). With the new planets, Gliese 667C would be the star with most known low-mass planets in its habitable zone,.[16] The five first signals also match the five stronger signals reported by Phil Gregory in his preliminary solution proposed in December 2012[10] and listed in the six-planet solution section. The last two candidates (Gliese 667Cg and h) are less certain and rely on the assumption of dynamical stability of the system.

However, one follow-up study found the confident evidence of the first two planets discovered with some evidence of the Gliese 667 Cd without finding any additional signals.[8]


  1. ^ a b c d e van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, arXiv:0708.1752, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357 
  2. ^ a b c d Pasinetti Fracassini, L. E. et al. (February 2001), "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS) - Third edition - Comments and statistics", Astronomy and Astrophysics 367: 521–524, arXiv:astro-ph/0012289, Bibcode:2001A&A...367..521P, doi:10.1051/0004-6361:20000451  Note: see VizieR catalogue J/A+A/367/521.
  3. ^ "Toward spectral classification of L and T dwarfs: infrared and optical spectroscopy and analysis", The Astrophysical Journal (The American Astronomical Society), January 2002, retrieved 2012-02-14 
  4. ^ a b c d e f g h i j k l m n Anglada-Escude, Guillem et al. (February 2012), "A planetary system around the nearby M dwarf GJ 667C with at least one super-Earth in its habitable zone", The Astrophysical Journal Letters, accepted, arXiv:/1202.0446, Bibcode:2012arXiv1202.0446A 
  5. ^ "The Colour of Stars", Australia Telescope, Outreach and Education (Commonwealth Scientific and Industrial Research Organisation), December 21, 2004, archived from the original on 2012-10-14, retrieved 2012-01-16 
  6. ^ Tokovinin, A. (September 2008), "Comparative statistics and origin of triple and quadruple stars", Monthly Notices of the Royal Astronomical Society 389 (2): 925–938, arXiv:0806.3263, Bibcode:2008MNRAS.389..925T, doi:10.1111/j.1365-2966.2008.13613.x 
  7. ^ a b c d e f g h i Anglada-Escudé, Guillem; Tuomi, Mikko; Gerlach, Enrico; Barnes, Rory; Heller, René; Jenkins, James S.; Wende, Sebastian; Vogt, Steven S.; Butler, R. Paul; Reiners, Ansgar; Jones, Hugh R. A. (2013-06-07). "A dynamically-packed planetary system around GJ 667C with three super-Earths in its habitable zone". Astronomy & Astrophysics. arXiv:1306.6074. Bibcode:2013A&A...556A.126A. doi:10.1051/0004-6361/201321331. Archived from the original on 2013-06-30. Retrieved 2013-06-25. 
  8. ^ a b c Feroz, F.; Hobson, M. P. (2014). "Bayesian analysis of radial velocity data of GJ667C with correlated noise: evidence for only two planets". Monthly Notices of the Royal Astronomical Society 437 (4): 3540–3549. arXiv:1307.6984. Bibcode:2014MNRAS.437.3540F. 
  9. ^ Abe, Y.; Abe-Ouchi, A.; Sleep, N. H.; Zahnle, K. J. (2011). "Habitable Zone Limits for Dry Planets". Astrobiology 11 (5): 443–460. Bibcode:2011AsBio..11..443A. doi:10.1089/ast.2010.0545. PMID 21707386.  edit
  10. ^ a b c d Philip C. Gregory. Additional Keplerian Signals in the HARPS data for Gliese 667C from a Bayesian Re-analysis. arXiv:1212.4058. Bibcode:2012arXiv1212.4058G. 
  11. ^ Bonfils, X. et al. (November 2011), "The HARPS search for southern extra-solar planets XXXI. The M-dwarf sample", Astronomy and Astrophysics, submitted, arXiv:/1111.5019, Bibcode:2011arXiv1111.5019B 
  12. ^ University of Göttingen. Presseinformation: Wissenschaftler entdecken möglicherweise bewohnbare Super-Erde - Göttinger Astrophysiker untersucht Planeten in 22 Lichtjahren Entfernung. Nr. 17/2012 - 02.02.2012. Announcement on university homepage, retrieved 2012-02-02
  13. ^ a b Chow, Denise (February 2, 2012). "Newfound Alien Planet is Best Candidate Yet to Support Life, Scientists Say". Archived from the original on 2013-04-19. Retrieved February 3, 2012. 
  14. ^ Sven Wedemeyer-Böhm. "Life on Gliese 667Cc?". Institute of Theoretical Astrophysics. 
  15. ^ Dvorsky, George (18 December 2012). "Astronomer discovers three potentially habitable planets orbiting around one red dwarf". io9. Archived from the original on 2013-07-03. Retrieved 21 March 2013. 
  16. ^ Kramer, Miriam (25 June 2013). "Found! 3 Super-Earth Planets That Could Support Alien Life". TechMediaNetwork. Archived from the original on 2013-06-29. Retrieved 2013-06-26. 

External links[edit]

Coordinates: Sky map 17h 18m 57.16483s, +34° 59′ 23.1416″