Gliese 176
Observation data Epoch J2000.0 Equinox J2000.0 | |
---|---|
Constellation | Taurus |
Right ascension | 04h 42m 55.7749s[1] |
Declination | +18° 57′ 29.399″[1] |
Apparent magnitude (V) | 9.95 |
Characteristics | |
Spectral type | M2V[2] |
B−V color index | 1.523 ± 0.025[3] |
Variable type | BY Dra |
Astrometry | |
Radial velocity (Rv) | 26.4105 ± 0.0004[2] km/s |
Proper motion (μ) | RA: 656.744±0.166[1] mas/yr Dec.: −1116.790±0.104[1] mas/yr |
Parallax (π) | 106.32 ± 0.60 mas[1] |
Distance | 30.7 ± 0.2 ly (9.41 ± 0.05 pc) |
Absolute magnitude (MV) | 10.10 ± 0.06[2] |
Details | |
Mass | 0.50 ± 0.03[4] M☉ |
Radius | 0.4525±0.0221[5] R☉ |
Luminosity | 0.0337±0.0018[5] L☉ |
Temperature | 3679±77[5] K |
Metallicity [Fe/H] | –0.1 ± 0.2[2] dex |
Rotation | 40.00 ± 0.11[2] days |
Rotational velocity (v sin i) | ≤0.8[2] km/s |
Age | 0.56 Gyr |
Other designations | |
Database references | |
SIMBAD | data |
Gliese 176 is a red dwarf in the constellation of Taurus. Based upon parallax measurements from the Hipparcos mission, it is located approximately 30 light-years away.[1] The star is orbited by a Super-Earth.
Planetary system
A planetary companion to Gliese 176 was announced in 2008.[6] Radial velocity observations with the Hobby-Eberly Telescope (HET) showed a 10.24-day periodicity, which was interpreted as being caused by a planet. With a semi-amplitude of 11.6 m/s, its minimum mass equated to 24.5 Earth masses, or approximately 1.4 Neptune masses.
Observations with the HARPS spectrograph could not confirm the 10.24-day variation.[2] Instead, two other periodicities were detected at 8.78 and 40.0 days, with amplitudes below the HET observational errors. The 40-day variation coincides with the rotational period of the star and is therefore caused by activity, but the shorter-period variation is not explained by activity and is therefore caused by a planet. Its semi-amplitude of 4.1 m/s corresponds to a minimum mass of 8.4 Earth masses, making the planet a Super-Earth.
In an independent study, observations with Keck-HIRES also failed to confirm the 10.24-day signal.[7] An 8.77-day periodicity - corresponding to the planet announced by the HARPS team - was detected to intermediate significance, though it was not deemed significant enough to claim a planetary cause with their data alone.
Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
---|---|---|---|---|---|---|
b | ≥9.06+1.54 −0.70 M🜨 |
0.066±0.001 | 8.776+0.001 −0.002 |
0.148+0.249 −0.036 |
— | — |
See also
References
- ^ a b c d e f Brown, A. G. A.; et al. (2016). "Gaia Data Release 1. Summary of the astrometric, photometric, and survey properties". Astronomy and Astrophysics. 595. A2. arXiv:1609.04172. Bibcode:2016A&A...595A...2G. doi:10.1051/0004-6361/201629512.Gaia Data Release 1 catalog entry
- ^ a b c d e f g Forveille, T.; et al. (2009). "The HARPS search for southern extra-solar planets. XIV. Gl 176b, a super-Earth rather than a Neptune, and at a different period". Astronomy and Astrophysics. 493 (2): 645–650. arXiv:0809.0750. Bibcode:2009A&A...493..645F. doi:10.1051/0004-6361:200810557.
- ^ 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.
- ^ Neves, V.; et al. (March 2013). "Metallicity of M dwarfs. III. Planet-metallicity and planet-stellar mass correlations of the HARPS GTO M dwarf sample". Astronomy and Astrophysics. 551. arXiv:1212.3372. Bibcode:2013A&A...551A..36N. doi:10.1051/0004-6361/201220574.
- ^ a b c von Braun, Kaspar; et al. (2014). "Stellar diameters and temperatures - V. 11 newly characterized exoplanet host stars". Monthly Notices of the Royal Astronomical Society. 438 (3): 2413–2425. arXiv:1312.1792. Bibcode:2014MNRAS.438.2413V. doi:10.1093/mnras/stt2360.
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: CS1 maint: unflagged free DOI (link) - ^ Endl, Michael; et al. (2008). "An m sin i = 24 M⊕ Planetary Companion to the Nearby M Dwarf GJ 176". The Astrophysical Journal. 673 (2): 1165–1168. arXiv:0709.0944. Bibcode:2008ApJ...673.1165E. doi:10.1086/524703.
- ^ Butler, R. Paul; et al. (2009). "Nondetection of the Neptune-Mass Planet Reported Around GJ 176". The Astrophysical Journal. 691 (2): 1738–1743. Bibcode:2009ApJ...691.1738B. doi:10.1088/0004-637X/691/2/1738.
- ^ Trifonov, T.; et al. (2018). "The CARMENES search for exoplanets around M dwarfs. First visual-channel radial-velocity measurements and orbital parameter updates of seven M-dwarf planetary systems". Astronomy and Astrophysics. 609. A117. arXiv:1710.01595. Bibcode:2018A&A...609A.117T. doi:10.1051/0004-6361/201731442.