Gliese 676

Not to be confused with Gliese 674.
Gliese 676 A/B
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Ara
Right ascension 17h 30m 11.20s[1]
Declination –51° 38′ 13.1″[1]
Apparent magnitude (V) 9.59
Characteristics
Spectral type M0V[2]/M3V
Apparent magnitude (B) 11.05/14.8
Apparent magnitude (J) 6.711
Apparent magnitude (H) 6.082
Apparent magnitude (K) 5.825
B−V color index 1.46
Astrometry
Proper motion (μ) RA: −260.02±1.34[1] mas/yr
Dec.: −184.29±0.82[1] mas/yr
Parallax (π)60.79 ± 1.62[1] mas
Distance54 ± 1 ly
(16.5 ± 0.4 pc)
Absolute magnitude (MV)8.55
Details
Mass0.71±0.04[3][4]/0.29[3] M☉
Luminosity0.082[3] L☉
Metallicity [Fe/H]0.23±0.10[3] dex
Rotation41.2±3.8 d[2]
Other designations
CD–51°10924, HIP 85647, LTT 6947/6948, NLTT 44859, NSV 8846
Database references
SIMBADdata
Exoplanet Archivedata
Extrasolar Planets
Encyclopaedia		data

Gliese 676 is a 10th-magnitude wide binary system of red dwarfs that has an estimated minimum separation of 800 AU with an orbital period of greater than 20,000 years.[4] It is located approximately 54 light years away in the constellation Ara. In 2009, a gas giant was found in orbit around the primary star, in addition to its confirmation in 2011 there was also a strong indication of a companion; the second gas giant was characterised in 2012, along with two much smaller planets.

Planetary system

The first planet discovered, b, is a super-jovian first characterised in October 2009. The planet was formally announced in 2011,[3] along with the first recognition of a trend not attributable to the companion star. Even after fitting a planet and a trend, it was noted that the residual velocities were still around 3.4 m/s, significantly larger than the instrumental errors of around 1.7 m/s. This tentatively implied the existence of other bodies in orbit, though nothing more could be said at the time.[3]

The star was a test case for the HARPS-TERRA software for better reduction of data from the HARPS spectrometer in early 2012.[5] Even with significantly lower margins of error on the data, less data was accessible than what was used in 2011. Still, the team reached a very similar conclusion to the previous team with a model of a planet and a trend. The residual velocities were still somewhat excessive, giving more weight to the existence of other bodies in the system, though still no conclusions could be made.

Between the time of the previous analysis and June 2012, the rest of the radial-velocity measurements used in 2011 were made public,[4] allowing them to be reduced using HARPS-TERRA. These were then analysed via a Bayesian probability analysis, which was previously used to discover HD 10180 i and j, which confirmed planet b and made a first characterisation of planet c, which was previously only described as a trend. After the first two signals were introduced, the next most powerful signal was at around 35.5 days, with an analytic false alarm probability of 0.156. Through 104 trials, the false alarm probability was found to be 0.44%, low enough for it to be included as a periodic, planetary signal. With a minimum mass of around 11 Earths, the planet lies at the accepted border between Super-Earths and gaseous, Neptune-like bodies of 10 Earths. After accepting the third signal, a strong peak at 3.6 days became apparent. With a false alarm probability much lower than that of the previously accepted body, it was immediately accepted. With a minimum mass of around 4.5 Earths, it is a small Super-Earth.

This system holds the current record for the widest range of masses in a single planetary system,[4] and also shows a hierarchy reminiscent of the solar system, with the gas giants at large distances from the star while the smaller bodies are much closer-in.

The Gliese 676 A planetary system[4]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
d ≥ 4.4±0.7 M⊕ 0.0413±0.0014 3.6000±0.0008 0.15±0.09 — —
e ≥ 11.5±1.5 M⊕ 0.187±0.007 35.37±0.07 0.24±0.12 — —
b ≥ 4.95±0.31 MJ 1.80±0.07 1050.3±1.2 0.328±0.004 — —
c ≥3 MJ 5.2 4400 0.2 — —

See also

References

  1. 1 2 3 4 5 van Leeuwen, F. (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. Vizier catalog entry
  2. 1 2 Suárez Mascareño, A.; et al. (September 2015), "Rotation periods of late-type dwarf stars from time series high-resolution spectroscopy of chromospheric indicators", Monthly Notices of the Royal Astronomical Society 452 (3): 2745−2756, arXiv:1506.08039, Bibcode:2015MNRAS.452.2745S, doi:10.1093/mnras/stv1441.
  3. 1 2 3 4 5 6 Forveille, T.; et al. (2011). "The HARPS search for southern extrasolar planets XXVI. Two giant planets around M0 dwarfs". Astronomy and Astrophysics 526. A141. arXiv:1012.1168. Bibcode:2011A&A...526A.141F. doi:10.1051/0004-6361/201016034.
  4. 1 2 3 4 5 Anglada-Escudé, Guillem; Tuomi, Mikko (2012). "A planetary system with gas giants and super-Earths around the nearby M dwarf GJ 676A. Optimizing data analysis techniques for the detection of multi-planetary systems". arXiv:1206.7118. Bibcode:2012A&A...548A..58A. doi:10.1051/0004-6361/201219910.
  5. ↑ Anglada-Escudé, Guillem; Butler, R. Paul (2012). "The HARPS-TERRA Project. I. Description of the Algorithms, Performance, and New Measurements on a Few Remarkable Stars Observed by HARPS". arXiv:1202.2570. Bibcode:2012ApJS..200...15A. doi:10.1088/0067-0049/200/2/15.

Coordinates: 17h 30m 11.2042s, −51° 38′ 13.116″

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