GU Piscium is a star in the constellation Pisces.[5] An RS Canum Venaticorum variable, it ranges from magnitude 12.96 to 13.24 over 1.04 days.[6] It is 48 Parsecs (155 light-years) distant from Earth.[7] This star is also believed to be a member of the AB Doradus moving group with a membership probability of 96.9%.[8]
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Pisces |
| Right ascension | 01h 12m 35.0519s[1] |
| Declination | 17° 03′ 55.5712″[1] |
| Apparent magnitude (V) | 12.96 - 13.24 |
| Characteristics | |
| Spectral type | M3[2] |
| Astrometry | |
| Radial velocity (Rv) | −1.5±0.5[3] km/s |
| Proper motion (μ) | RA: 96.642±0.127[1] mas/yr Dec.: −100.704±0.107[1] mas/yr |
| Parallax (π) | 21.0019 ± 0.0721 mas[1] |
| Distance | 155.3 ± 0.5 ly (47.6 ± 0.2 pc) |
| Details | |
| Radius | 0.54±0.04[4] R☉ |
| Surface gravity (log g) | 4.75±0.07[4] cgs |
| Temperature | 3250±32[4] K |
| Metallicity | −0.25±0.19[4] |
| Rotational velocity (v sin i) | 23.7±2.2[3] km/s |
| Other designations | |
| Database references | |
| SIMBAD | data |
Planetary system edit
In 2014, it was found to have a gas giant planet—GU Piscium b—orbiting it.[7]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | 9–13 MJ MJ | 2000 | 163,000 | — | — | — |
References edit
- ^ a b c d e Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
- ^ Riaz, Basmah; Gizis, John E.; Harvin, James (2006). "Identification of New M Dwarfs in the Solar Neighborhood". The Astronomical Journal. 132 (2): 866–872. arXiv:astro-ph/0606617. Bibcode:2006AJ....132..866R. doi:10.1086/505632. S2CID 6282011.
- ^ a b Malo, Lison; et al. (2014). "BANYAN. III. Radial Velocity, Rotation, and X-Ray Emission of Low-mass Star Candidates in Nearby Young Kinematic Groups". The Astrophysical Journal. 788 (1). 81. arXiv:1402.6053. Bibcode:2014ApJ...788...81M. doi:10.1088/0004-637X/788/1/81. S2CID 119276883.
- ^ a b c d Malo, Lison; et al. (2014). "BANYAN. IV. Fundamental Parameters of Low-mass Star Candidates in Nearby Young Stellar Kinematic Groups—Isochronal Age Determination using Magnetic Evolutionary Models". The Astrophysical Journal. 792 (1). 37. arXiv:1406.6750. Bibcode:2014ApJ...792...37M. doi:10.1088/0004-637X/792/1/37. S2CID 96438831.
- ^ a b "V* GU Psc". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-10-06.
- ^ BSJ (11 November 2011). "GU Piscium". AAVSO Website. American Association of Variable Star Observers. Retrieved 5 July 2014.
- ^ a b Naud, Marie-Eve; et al. (2014). "Discovery of a Wide Planetary-Mass Companion to the Young M3 Star Gu Psc". The Astrophysical Journal. 787 (1). 5. arXiv:1405.2932. Bibcode:2014ApJ...787....5N. doi:10.1088/0004-637X/787/1/5. S2CID 35264096.
- ^ Malo, Lison; et al. (2013). "Bayesian Analysis to Identify New Star Candidates in Nearby Young Stellar Kinematic Groups". The Astrophysical Journal. 762 (2). 88. arXiv:1209.2077. Bibcode:2013ApJ...762...88M. doi:10.1088/0004-637X/762/2/88. S2CID 118497872.