Pi Piscium
  | |
| Observation data EpochJ2000.0EquinoxJ2000.0(ICRS) | |
|---|---|
| Constellation | Pisces |
| Right ascension | 01h37m05.91523s[1] |
| Declination | +12° 08′ 29.5186″[1] |
| Apparent magnitude(V) | 5.60[2] |
| Characteristics | |
| Spectral type | F0 V[3] |
| Astrometry | |
| Radial velocity(Rv) | −1.0[2]km/s |
| Proper motion(μ) | RA:−77.29[1]mas/yr Dec.:+9.13[1]mas/yr |
| Parallax(π) | 28.50 ± 0.97mas[1] |
| Distance | 114 ± 4ly (35 ± 1pc) |
| Absolute magnitude(MV) | +2.94[2] |
| Details | |
| Mass | 1.51±0.02[4]M☉ |
| Luminosity | 6.3[4]L☉ |
| Surface gravity(logg) | 4.00[2]cgs |
| Temperature | 6,850[2]K |
| Metallicity[Fe/H] | −0.45±0.05[5]dex |
| Rotational velocity(vsini) | 105.9[2]km/s |
| Age | 2.0[6]Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Pi Piscium(π Piscium) is a solitary,[8]yellow-white huedstarin thezodiacconstellationofPisces.It is faintly visible to the naked eye, having anapparent visual magnitudeof 5.60.[2]Based upon an annualparallax shiftof 28.50masas seen from Earth,[1]it is located about 1114light yearsfrom theSun.It is a member of thethin diskpopulation of theMilky Way.[5]
This is an ordinaryF-type main-sequence starwith astellar classificationof F0 V.[3]At the estimated age of two billion years,[6]it is about 55% of the way through itsmain sequencelifetime[4]and still has a relatively high rate of spin with aprojected rotational velocityof 105.9 km/s.[2]The star has 1.5[4]times themass of the Sunand is radiating 6.3[4]times theSun's luminosityat aneffective temperatureof 6,850 K.[2]
Naming
[edit]InChinese,Hữu càng(Yòu Gèng), meaningOfficial in Charge of the Pasturing,refers to an asterism consisting of refers to an asterism consisting of π Piscium,η Piscium,ρ Piscium,ο Pisciumand104 Piscium.Consequently, theChinese namefor π Piscium itself isHữu càng tam(Yòu Gèng sān,English:the Third Star of Official in Charge of the Pasturing.)[9]
References
[edit]- ^abcdefvan 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,S2CID18759600.
- ^abcdefghiPaunzen, 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,S2CID56332289,A67.
- ^abCowley, 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.
- ^abcdeZorec, 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,S2CID55586789.
- ^abRamírez, 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,S2CID119199829.
- ^abHolmberg, 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,S2CID118577511.
- ^"pi. Psc".SIMBAD.Centre de données astronomiques de Strasbourg.Retrieved2017-07-25.
{{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,S2CID14878976.
- ^(in Chinese)AEEA (Activities of Exhibition and Education in Astronomy) thiên văn giáo dục tin tức võng 2006 năm 5 nguyệt 19 ngày
