Star in the constellation Pisces
Omicron Piscium
Location of ο Piscium (circled)
Observation dataEpoch J2000.0 Equinox J2000.0 (ICRS )
Constellation
Pisces
Right ascension 01h 45m 23.63185s [ 1]
Declination
+09° 09′ 27.8530″[ 1]
Apparent magnitude (V)4.27[ 2]
Characteristics
Evolutionary stage
Horizontal branch [ 3]
Spectral type
K0 III[ 2]
U−B color index
+0.736[ 4]
B−V color index
+0.959[ 4]
Astrometry Proper motion (μ) RA: +72.98[ 1] mas /yr Dec.: +39.30[ 1] mas /yr Parallax (π)11.67 ± 0.67 mas [ 1] Distance 280 ± 20 ly pc ) Absolute magnitude (MV )−0.22[ 2] Details[ 5] Mass 3.03 M ☉ Radius ± 0.21[ 6] R ☉ Luminosity 132 L ☉ Surface gravity (log g )2.57 cgs Temperature 5,004 K Metallicity 0.10 dex Rotational velocity (v sin i )2.88 km/s Age 390 Myr Other designations Torcular, Torcularis Septentrionalis,
ο Psc ,
110 Piscium ,
BD +08° 273,
FK5 60,
GC 2139,
HD 10761,
HIP 8198,
HR 510,
SAO 110110,
PPM 144950
[ 7] Database references SIMBAD data
Omicron Piscium (ο Piscium , abbreviated Omi Psc , ο Psc ) is a binary star in the constellation of Pisces . It is visible to the naked eye, having an apparent visual magnitude of 4.27.[ 2] parallax shift of 11.67 mas as seen from the Earth,[ 1] light-years from the Sun . It is positioned near the ecliptic , so it can be occulted by the Moon and (very rarely) by planets. [ 8] Newfoundland and the Atlantic Ocean .[ 9] : 165 thin disk population of the Milky Way .[ 5]
The two components are designated Omicron Piscium A (formally named Torcular )[ 10]
Nomenclature
ο Piscium (Latinised to Omicron Piscium ) is the system's Bayer designation . The designations of the two components as Omicron Piscium A and B derives from the convention used by the Washington Multiplicity Catalog (WMC) for multiple star systems , and adopted by the International Astronomical Union (IAU).[ 11]
The system bore the traditional name Torcularis septentrionalis , taken from the 1515 Almagest . The name is translated from the Greek ληνός ('full'), which was "erroneously written for λίνος" ('linen').[ 12] Working Group on Star Names (WGSN)[ 13] multiple systems .[ 14] Torcular for the component Omicron Piscium A on 5 September 2017 and it is now so included in the List of IAU-approved Star Names.[ 10]
In Chinese , 右更 Yòu Gèng Official in Charge of the Pasturing asterism consisting of Omicron Piscium, Eta Piscium , Rho Piscium , Pi Piscium and 104 Piscium . Consequently, the Chinese name for Omicron Piscium itself is 右更四 Yòu Gèng sì the Fourth Star of Official in Charge of the Pasturing .)[ 15]
Properties
This is a probable astrometric binary system.[ 16] evolved K-type giant star with a stellar classification of K0 III.[ 2] [ 5] horizontal branch , rather than the red-giant branch .[ 17] red clump star that is generating energy through helium fusion at its core.[ 3] mass of the Sun and has expanded to over 14 times the Sun's radius . It is radiating 132 times the Sun's luminosity from its photosphere at an effective temperature of 5,004 K.[ 5]
References
^ a b c d e f 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 . ^ a b c d e Setiawan, J.; et al. (July 2004), "Precise radial velocity measurements of G and K giants. Multiple systems and variability trend along the Red Giant Branch", Astronomy and Astrophysics , 421 : 241– 254, Bibcode :2004A&A...421..241S , doi :10.1051/0004-6361:20041042-1 ^ a b Alves, David R. (August 2000), "K-Band Calibration of the Red Clump Luminosity", The Astrophysical Journal , 539 (2): 732– 741, arXiv :astro-ph/0003329 Bibcode :2000ApJ...539..732A , doi :10.1086/309278 , S2CID 16673121 . ^ a b Jennens, P. A.; Helfer, H. L. (September 1975), "A new photometric metal abundance and luminosity calibration for field G and K giants", Monthly Notices of the Royal Astronomical Society 172 (3): 667– 679, Bibcode :1975MNRAS.172..667J , doi :10.1093/mnras/172.3.667 ^ a b c d Jofré, E.; et al. (2015), "Stellar parameters and chemical abundances of 223 evolved stars with and without planets", Astronomy & Astrophysics , 574 : A50, arXiv :1410.6422 Bibcode :2015A&A...574A..50J , doi :10.1051/0004-6361/201424474 , S2CID 53666931 . ^ Baines, Ellyn K.; Blomquist, Solvay; Clark III, James H.; Gorney, Jim; Maier, Erin; Sanborn, Jason; Schmitt, Henrique R.; Stone, Jordan M.; van Belle, Gerard T.; Braun, Kaspar von (2023-01-09). "Simultaneous Six-way Observations from the Navy Precision Optical Interferometer" . The Astronomical Journal . 165 (2): 41. Bibcode :2023AJ....165...41B . doi :10.3847/1538-3881/aca277 ISSN 0004-6256 . ^ "omi Psc" . SIMBAD Centre de données astronomiques de Strasbourg . Retrieved 2017-07-25 .^ Richichi, A.; et al. (January 2016), "Lunar Occultations of 18 Stellar Sources from the 2.4 m Thai National Telescope", The Astronomical Journal , 151 (1): 5, Bibcode :2016AJ....151...10R , doi :10.3847/0004-6256/151/1/10 S2CID 119258140 , 10. ^ Meeus, Jan (2002). "Mutual occultations of planets". More Mathematical Astronomy Morsels (PDF) . pp. 174– 185. ISBN 0943396743 ^ a b "Naming Stars" . IAU.org. Retrieved 16 December 2017 .^ Hessman, F. V.; Dhillon, V. S.; Winget, D. E.; Schreiber, M. R.; Horne, K.; Marsh, T. R.; Guenther, E.; Schwope, A.; Heber, U. (2010). "On the naming convention used for multiple star systems and extrasolar planets". arXiv :1012.0707 astro-ph.SR ]. ^ Allen, Richard Hinckley (1963), "Pisces, the Fishes" , Star Names — Their Lore and Meaning , Dover ^ "IAU Working Group on Star Names (WGSN)" . Retrieved 22 May 2016 .^ "WG Triennial Report (2015-2018) - Star Names" (PDF) . p. 5. Retrieved 2018-07-14 .^ "AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網" (in Chinese). 2006-05-19. Archived from the original on 2016-03-03. Retrieved 2012-08-30 .^ 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 . ^ Reffert, Sabine; et al. (2015), "Precise radial velocities of giant stars. VII. Occurrence rate of giant extrasolar planets as a function of mass and metallicity", Astronomy and Astrophysics , 574A (2): 116– 129, arXiv :1412.4634 Bibcode :2015A&A...574A.116R , doi :10.1051/0004-6361/201322360 , S2CID 59334290 .
