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Lambda Piscium

From Wikipedia, the free encyclopedia
Star in the constellation Pisces
Lambda Piscium
Location of λ Piscium (circled)
Observation data
EpochJ2000.0      EquinoxJ2000.0 (ICRS)
ConstellationPisces
Right ascension23h 42m 02.80612s[1]
Declination+01° 46′ 48.1484″[1]
Apparent magnitude (V)4.49[2]
Characteristics
Spectral typeA7 V[3]
U−Bcolor index+0.09[2]
B−Vcolor index+0.20[2]
Astrometry
Radial velocity (Rv)6.7[4] km/s
Proper motion (μ)RA: −129.70[1]mas/yr
Dec.: −154.80[1]mas/yr
Parallax (π)30.59±0.19 mas[1]
Distance106.6 ± 0.7 ly
(32.7 ± 0.2 pc)
Absolute magnitude (MV)+1.92[5]
Details
Mass1.806[3] M
Radius2.0403±0.0451[3] R
Luminosity13.3897±0.1692[3] L
Surface gravity (log g)4.08[4] cgs
Temperature7,734±80[3] K
Metallicity[Fe/H]0.02[4] dex
Rotational velocity (v sin i)70[6] km/s
Age583±20[6] Myr
Other designations
λ Psc,18 Piscium,BD+00°5037,FK5 1620,HD 222603,HIP 116928,HR 8984,SAO 128336[7]
Database references
SIMBADdata

Lambda Piscium,Latinized fromλ Piscium, is a solitary,[8] white-huedstar in thezodiacconstellation ofPisces. With anapparent visual magnitude of 4.49,[2] it is visible to the naked eye, forming the southeast corner of the "Circlet"asterism in Pisces. Based upon a measured annualparallax shift of 30.59 mas as seen from Earth,[1] it is located 107 light years distant from theSun. Lambda Piscium is a member of theUrsa Major Stream, lying among the outer parts, or corona, of thismoving group of stars that roughly follow a common heading through space.[9]

This well-studied star[4] has astellar classification A7 V,[3] indicating it is anA-type main-sequence star that is generating energy throughhydrogen fusion at itscore. It has 1.8 times themass of the Sun and double theSun's radius. The star is radiating 13.3 times theSun's luminosity from itsphotosphere at aneffective temperature of 7,734 K.[3] Lambda Piscium is around 583 million years old and is spinning with aprojected rotational velocity of 70 km/s.[6]

Naming

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InChinese,雲雨 (Yún Yǔ), meaningCloud and Rain, refers to an asterism consisting of λ Piscium,κ Piscium,12 Piscium and21 Piscium. Consequently, theChinese name for λ Piscium itself is雲雨四 (Yún Yǔ sì, English:the Fourth Star of Cloud and Rain.)[10]

References

[edit]
  1. ^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,S2CID 18759600.
  2. ^abcdArgue, A. N. (1966), "UBV photometry of 550 F, G and K type stars",Monthly Notices of the Royal Astronomical Society,133 (4):475–493,Bibcode:1966MNRAS.133..475A,doi:10.1093/mnras/133.4.475.
  3. ^abcdefgBoyajian, Tabetha S.; et al. (July 2013), "Stellar Diameters and Temperatures. III. Main-sequence A, F, G, and K Stars: Additional High-precision Measurements and Empirical Relations",The Astrophysical Journal,771 (1): 31,arXiv:1306.2974,Bibcode:2013ApJ...771...40B,doi:10.1088/0004-637X/771/1/40,S2CID 14911430, 40. See Table 3.
  4. ^abcdGebran, M.; et al. (May 2016), "A new method for the inversion of atmospheric parameters of A/Am stars",Astronomy & Astrophysics,589: 10,arXiv:1603.01146,Bibcode:2016A&A...589A..83G,doi:10.1051/0004-6361/201528052,S2CID 118549566, A83.
  5. ^Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation",Astronomy Letters,38 (5): 331,arXiv:1108.4971,Bibcode:2012AstL...38..331A,doi:10.1134/S1063773712050015,S2CID 119257644.
  6. ^abcZorec, 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.
  7. ^"lam Psc".SIMBAD.Centre de données astronomiques de Strasbourg. Retrieved2017-07-25.{{cite web}}: CS1 maint: postscript (link)
  8. ^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.
  9. ^Chupina, N. V.; et al. (June 2006), "Kinematic structure of the corona of the Ursa Major flow found using proper motions and radial velocities of single stars",Astronomy and Astrophysics,451 (3):909–916,Bibcode:2006A&A...451..909C,doi:10.1051/0004-6361:20054009.
  10. ^(in Chinese)AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 8 日Archived 2012-04-15 at theWayback Machine
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