Astronomy:Gliese 176
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Taurus |
| Right ascension | 04h 42m 55.7750s[1] |
| Declination | +18° 57′ 29.396″[1] |
| Apparent magnitude (V) | 9.95[2] |
| Characteristics | |
| Spectral type | M2V[3] |
| B−V color index | 1.523±0.025[4] |
| Variable type | None[5] |
| Astrometry | |
| Radial velocity (Rv) | 26.4105±0.0004[3] km/s |
| Proper motion (μ) | RA: +656.647[1] mas/yr Dec.: −1116.594[1] mas/yr |
| Parallax (π) | 105.4275 ± 0.0210[1] mas |
| Distance | 30.937 ± 0.006 ly (9.485 ± 0.002 pc) |
| Absolute magnitude (MV) | 10.10±0.06[3] |
| Details | |
| Mass | 0.485±0.012[6] M☉ |
| Radius | 0.474±0.015[6] R☉ |
| Luminosity | 0.03516±0.00032[6] L☉ |
| Temperature | 3,632+58 −56[6] K |
| Metallicity [Fe/H] | −0.1±0.2[3] dex |
| Rotation | 40.00±0.11[3] days |
| Rotational velocity (v sin i) | ≤0.8[3] km/s |
| Age | 8.8+2.5 −2.8[5] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
| Extrasolar Planets Encyclopaedia | data |
Gliese 176 is a small star with an orbiting exoplanet in the constellation of Taurus. With an apparent visual magnitude of 9.95,[2] it is too faint to be visible to the naked eye. It is located at a distance of 30.9 light years based on parallax measurements,[1] and is drifting further away with a heliocentric radial velocity of 26.4 km/s.[3]
This is an M-type main-sequence star, sometimes called a red dwarf, with a stellar classification of M2V.[3] It has 49% of the Sun's mass and 47% of the radius of the Sun. The star is radiating just 3.5% of the luminosity of the Sun from its photosphere at an effective temperature of 3,632 K. It is estimated to be around nine billion years old,[5] and is spinning slowly with a rotation period of 40 days. The star is orbited by a Super-Earth.
Planetary system
A planetary companion to Gliese 176 was announced in 2008.[7] 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.[3] 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.[8] 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
- List of extrasolar planets
- Gliese 674
References
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940 Gaia DR3 record for this source at VizieR.
- ↑ 2.0 2.1 Koen, C.; Kilkenny, D.; van Wyk, F.; Marang, F. (2010). "UBV(RI)C JHK observations of Hipparcos-selected nearby stars". Monthly Notices of the Royal Astronomical Society 403 (4): 1949–1968. doi:10.1111/j.1365-2966.2009.16182.x. Bibcode: 2010MNRAS.403.1949K.
- ↑ 3.0 3.1 3.2 3.3 3.4 3.5 3.6 3.7 3.8 Forveille, Thierry; Bonfils, Xavier; Delfosse, Xavier; Gillon, Michaël; Udry, Stéphane; Bouchy, François; Lovis, Christophe; Mayor, Michel 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. doi:10.1051/0004-6361:200810557. Bibcode: 2009A&A...493..645F. https://www.aanda.org/articles/aa/full/2009/02/aa10557-08/aa10557-08.html.
- ↑ van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics 474 (2): 653–664. doi:10.1051/0004-6361:20078357. Bibcode: 2007A&A...474..653V. http://www.aanda.org/index.php?option=com_article&access=bibcode&Itemid=129&bibcode=2007A%2526A...474..653VFUL.
- ↑ 5.0 5.1 5.2 Brown, Alexander et al. (May 2023). "Coronal X-Ray Emission from Nearby, Low-mass, Exoplanet Host Stars Observed by the MUSCLES and Mega-MUSCLES HST Treasury Survey Projects". The Astronomical Journal 165 (5): 195. doi:10.3847/1538-3881/acc38a. 195. Bibcode: 2023AJ....165..195B.
- ↑ 6.0 6.1 6.2 6.3 Pineda, J. Sebastian et al. (September 2021). "The M-dwarf Ultraviolet Spectroscopic Sample. I. Determining Stellar Parameters for Field Stars". The Astrophysical Journal 918 (1): 23. doi:10.3847/1538-4357/ac0aea. 40. Bibcode: 2021ApJ...918...40P.
- ↑ 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. doi:10.1086/524703. Bibcode: 2008ApJ...673.1165E.
- ↑ Butler, R. Paul et al. (2009). "Nondetection of the Neptune-Mass Planet Reported Around GJ 176". The Astrophysical Journal 691 (2): 1738–1743. doi:10.1088/0004-637X/691/2/1738. Bibcode: 2009ApJ...691.1738B.
- ↑ Trifonov, Trifon; Kürster, Martin; Zechmeister, Mathias; Tal-Or, Lev; Caballero, José A.; Quirrenbach, Andreas; Amado, Pedro J.; Ribas, Ignasi 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. doi:10.1051/0004-6361/201731442. Bibcode: 2018A&A...609A.117T.
Coordinates: 
04h 42m 55.78s, +18° 57′ 29.40″
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