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Iota Cephei

Coordinates:Sky map22h 49m 40.91s, +66° 12′ 2.6″
From Wikipedia, the free encyclopedia
Star in the constellation Cepheus
Iota Cephei
Observation data
EpochJ2000.0      EquinoxJ2000.0 (ICRS)
ConstellationCepheus
Right ascension22h 49m 40.817s[1]
Declination+66° 12′ 01.46″[1]
Apparent magnitude (V)3.507[2]
Characteristics
Spectral typeK0 III[3]
U−Bcolor index+0.924[2]
B−Vcolor index+1.053[2]
Astrometry
Radial velocity (Rv)−12.763±0.0008[4] km/s
Proper motion (μ)RA: −65.89[1]mas/yr
Dec.: −125.17[1]mas/yr
Parallax (π)28.29±0.10 mas[1]
Distance115.3 ± 0.4 ly
(35.3 ± 0.1 pc)
Absolute magnitude (MV)0.76[3]
Details[5]
Mass2.15±0.23 M
Radius11.08±0.16 R
Luminosity57.0±0.6 L
Surface gravity (log g)2.69±0.06 cgs
Temperature4,768±33 K
Metallicity [Fe/H]+0.05±0.10 dex
Rotational velocity (v sin i)10[6] km/s
Age1.2±0.6 Gyr
Other designations
ι Cep,32 Cep,BD+65°1814,HD 216228,HIP 112724,HR 8694,SAO 20268[7]
Database references
SIMBADdata

Iota Cephei (ι Cephei, ι Cep) is astar in the northernconstellationCepheus. Based upon an annualparallax shift of28.29 mas as seen from the Earth,[1] it is located about115 light years from theSun. The star is visible to the naked eye with anapparent visual magnitude of 3.5.[2]

It is aK-typegiant star with astellar classification of K0 III.[3] It is currently at anevolutionary stage known as thered clump, indicating that it is generating energy through the fusion ofhelium at its core.[8] It has 11 times the Sun's radius and about 2.15 times the mass of theSun. Its luminosity is 57 times that of the Sun, and its surface has aneffective temperature of 4,768 K.[5]

Pole star

[edit]

Iota Cephei is located within 5° of theprecessional path traced across thecelestial sphere by the Earth'sNorth pole. In about 3,000 years, it will be one of the closest visible stars to the celestial north pole, along withAlfirk which will also be within 5° of the precessional path, on the other side.

Preceded byPole StarSucceeded by
Errai5200AD to 7500AD
with
Alfirk
Alderamin

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. ^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. ^abcHekker, S.; et al. (August 2006), "Precise radial velocities of giant stars. I. Stable stars",Astronomy and Astrophysics,454 (3):943–949,arXiv:astro-ph/0604502,Bibcode:2006A&A...454..943H,doi:10.1051/0004-6361:20064946,S2CID 119529768.
  4. ^Brown, 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.
  5. ^abReffert, 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 & Astrophysics,574: A116,arXiv:1412.4634,Bibcode:2015A&A...574A.116R,doi:10.1051/0004-6361/201322360,hdl:10722/215277,S2CID 59334290.
  6. ^Bernacca, P. L.; Perinotto, M. (1970), "A catalogue of stellar rotational velocities",Contributi Osservatorio Astronomico di Padova in Asiago,239 (1): 1,Bibcode:1970CoAsi.239....1B.
  7. ^"iot Cep".SIMBAD.Centre de données astronomiques de Strasbourg. Retrieved2017-05-06.
  8. ^Tautvaišienė, G.; et al. (December 2010), "C, N and O abundances in red clump stars of the Milky Way",Monthly Notices of the Royal Astronomical Society,409 (3):1213–1219,arXiv:1007.4064,Bibcode:2010MNRAS.409.1213T,doi:10.1111/j.1365-2966.2010.17381.x,S2CID 119182458.


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