Location of π Piscium (circled) | |
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Pisces |
| Right ascension | 01 37 05.91523 |
| Declination | +12° 08′ 29.5186″ |
| Apparent magnitude (V) | 5.60 |
| Characteristics | |
| Spectral type | F0 V |
| Astrometry | |
| Radial velocity (Rv) | −1.0 km/s |
| Proper motion (μ) | RA: −77.29 mas/yr Dec.: +9.13 mas/yr |
| Parallax (π) | 28.50 ± 0.97 mas |
| Distance | 114 ± 4 ly (35 ± 1 pc) |
| Absolute magnitude (MV) | +2.94 |
| Details | |
| Mass | 1.51±0.02 M☉ |
| Luminosity | 6.3 L☉ |
| Surface gravity (log g) | 4.00 cgs |
| Temperature | 6,850 K |
| Metallicity | −0.45±0.05 dex |
| Rotational velocity (v sin i) | 105.9 km/s |
| Age | 2.0 Gyr |
| Other designations | |
| π Psc, 102 Piscium, BD+11° 205, FK5 1046, GC 1954, HD 9919, HIP 7535, HR 463, SAO 92536, PPM 117498 | |
| Database references | |
| SIMBAD | data |
Pi Piscium (π Piscium) is a solitary, yellow-white hued star in the zodiac constellation of Pisces. It is faintly visible to the naked eye, having an apparent visual magnitude of 5.60. Based upon an annual parallax shift of 28.50 mas as seen from Earth, it is located about 1114 light years from the Sun. It is a member of the thin disk population of the Milky Way.
This is an ordinary F-type main-sequence star with a stellar classification of F0 V. At the estimated age of two billion years, it is about 55% of the way through its main sequence lifetime and still has a relatively high rate of spin with a projected rotational velocity of 105.9 km/s. The star has 1.5 times the mass of the Sun and is radiating 6.3 times the Sun's luminosity at an effective temperature of 6,850 K.
Naming
In Chinese, 右更 (Yòu Gèng), meaning Official in Charge of the Pasturing, refers to an asterism consisting of refers to an asterism consisting of π Piscium, η Piscium, ρ Piscium, ο Piscium and 104 Piscium. Consequently, the Chinese name for π Piscium itself is 右更三 (Yòu Gèng sān, English: the Third Star of Official in Charge of the Pasturing.)
References
- ^ 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, S2CID 18759600.
- ^ Paunzen, E.; et al. (July 2014), "Investigating the possible connection between λ Bootis stars and intermediate Population II type stars", Astronomy & Astrophysics, 567: 8, arXiv:1406.3936, Bibcode:2014A&A...567A..67P, doi:10.1051/0004-6361/201423817, S2CID 56332289, A67.
- ^ Cowley, Anne; Fraquelli, Dorothy (February 1974), "MK Spectral Types for Some Bright F Stars", Publications of the Astronomical Society of the Pacific, 86 (509): 70, Bibcode:1974PASP...86...70C, doi:10.1086/129562.
- ^ Zorec, J.; Royer, F. (January 2012), "Rotational velocities of A-type stars. IV. Evolution of rotational velocities", Astronomy & Astrophysics, 537: A120, arXiv:1201.2052, Bibcode:2012A&A...537A.120Z, doi:10.1051/0004-6361/201117691, S2CID 55586789.
- ^ Ramírez, I.; et al. (September 2012), "Lithium Abundances in nearby FGK Dwarf and Subgiant Stars: Internal Destruction, Galactic Chemical Evolution, and Exoplanets", The Astrophysical Journal, 756 (1): 46, arXiv:1207.0499, Bibcode:2012ApJ...756...46R, doi:10.1088/0004-637X/756/1/46, S2CID 119199829.
- ^ Holmberg, J.; et al. (July 2009), "The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics", Astronomy and Astrophysics, 501 (3): 941–947, arXiv:0811.3982, Bibcode:2009A&A...501..941H, doi:10.1051/0004-6361/200811191, S2CID 118577511.
- "pi. Psc". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-07-25.
{{cite web}}: CS1 maint: postscript (link) - Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869–879, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.
- (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 5 月 19 日 Archived 2016-03-03 at the Wayback Machine
