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77 Aquarii

From Wikipedia, the free encyclopedia
Star in the constellation of Aquarius
77 Aquarii
Observation data
Epoch J2000      Equinox J2000
ConstellationAquarius
Right ascension22h 54m 45.47009s[1]
Declination–16° 16′ 19.0505″[1]
Apparent magnitude (V)5.55[2]
Characteristics
Evolutionary stagegiant
Spectral typeK1 III[3]
U−Bcolor index+1.089[2]
B−Vcolor index+1.104[2]
Variable typesuspected[4]
Astrometry
Radial velocity (Rv)−34.59±0.16[1] km/s
Proper motion (μ)RA: –222.505[1]mas/yr
Dec.: –88.355[1]mas/yr
Parallax (π)24.1777±0.1211 mas[1]
Distance134.9 ± 0.7 ly
(41.4 ± 0.2 pc)
Absolute magnitude (MV)2.46[5]
Details
Mass1.14[6] M
Radius5.79+0.22
−0.21
[1] R
Luminosity13.347±0.085[1] L
Surface gravity (log g)2.8[7] cgs
Temperature4,583+86
−83
[1] K
Metallicity [Fe/H]+0.03[7] dex
Rotational velocity (v sin i)3.9[7] km/s
Age7.61[6] Gyr
Other designations
70 Aqr,NSV 14358,BD−17°6619,HD 216640,HIP 113148,HR 8711,SAO 165376[8]
Database references
SIMBADdata

77 Aquarii is a single[9]star located 135 light years away from the Sun in theequatorialconstellation ofAquarius.77 Aquarii is itsFlamsteed designation. It is visible to the naked eye as a dim star with a baselineapparent visual magnitude of 5.55.[2] The star is moving closer to the Earth with a heliocentricradial velocity of −35 km/s.[1]

At the estimated age of 7.61[6] billion years old, this is an aginggiant star with astellar classification of K1 III.[3] It is a suspectedvariable star that ranges in brightness from a maximum of magnitude 5.53 down to 5.60.[4] 77 Aquarii has 1.14[6] times themass of the Sun and, after exhausting the hydrogen at itscore, has expanded to six times theSun's radius. It is radiating 13.3[1] times the Sun's luminosity from itsphotosphere at aneffective temperature of 4,581 K,[7] giving it the orange-hued glow of aK-type star.[10]

References

[edit]
  1. ^abcdefghijkBrown, 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 atVizieR.
  2. ^abcdJennens, 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.
  3. ^abHouk, Nancy; Smith-Moore, M. (1978),Michigan catalogue of two-dimensional spectral types for the HD stars, vol. 4, Ann Arbor: Dept. of Astronomy, University of Michigan,Bibcode:1988mcts.book.....H.
  4. ^abSamus, N. N.; et al. (2017), "General Catalogue of Variable Stars",Astronomy Reports, 5.1,61 (1):80–88,Bibcode:2017ARep...61...80S,doi:10.1134/S1063772917010085,S2CID 125853869.
  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. ^abcdWittenmyer, Robert A.; Liu, Fan; Wang, Liang; Casagrande, Luca; Johnson, John Asher; Tinney, C. G. (July 2016), "The Pan-Pacific Planet Search. V. Fundamental Parameters for 164 Evolved Stars",The Astronomical Journal,152 (1): 15,arXiv:1605.00323,Bibcode:2016AJ....152...19W,doi:10.3847/0004-6256/152/1/19,S2CID 55991800, 19.
  7. ^abcdMassarotti, Alessandro; et al. (January 2008), "Rotational and radial velocities for a sample of 761 HIPPARCOS giants and the role of binarity",The Astronomical Journal,135 (1):209–231,Bibcode:2008AJ....135..209M,doi:10.1088/0004-6256/135/1/209.
  8. ^"* 77 Aqr".SIMBAD.Centre de données astronomiques de Strasbourg. Retrieved2012-07-15.
  9. ^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.
  10. ^"The Colour of Stars",Australia Telescope, Outreach and Education,Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, archived fromthe original on March 18, 2012, retrieved2012-01-16

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