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79 Ceti

Coordinates:Sky map02h 35m 19.9283s, −03° 33′ 38.167″
From Wikipedia, the free encyclopedia
Binary star system in the constellation of Cetus
79 Ceti
Observation data
Epoch J2000.0      Equinox J2000.0
ConstellationCetus[1]
A
Right ascension02h 35m 19.9292s[2]
Declination−03° 33′ 38.173″[2]
Apparent magnitude (V)+6.83[1]
B
Right ascension02h 35m 19.8725s[3]
Declination−03° 33′ 44.340″[3]
Apparent magnitude (V)+14.4[4]
Characteristics
A
Evolutionary stagesubgiant[2]
Spectral typeG2V[5][6]
B−Vcolor index0.670±0.004[1]
B
Evolutionary stagemain sequence[7]
Spectral typeM2.5[7]
Astrometry
Radial velocity (Rv)−50.93±0.09[1] km/s
Absolute magnitude (MV)+3.88[1]
A
Proper motion (μ)RA: −155.501[2]mas/yr
Dec.: −437.848[2]mas/yr
Parallax (π)26.5057±0.0271 mas[2]
Distance123.1 ± 0.1 ly
(37.73 ± 0.04 pc)
B
Proper motion (μ)RA: −141.533[3]mas/yr
Dec.: −442.657[3]mas/yr
Parallax (π)26.5223±0.0353 mas[3]
Distance123.0 ± 0.2 ly
(37.70 ± 0.05 pc)
Details
79 Ceti A
Mass1.01[8] M
Radius1.48[9] R
Luminosity1.99±0.04[8] L
Surface gravity (log g)4.19±0.02[8] cgs
Temperature5,806±17[8] K
Metallicity[Fe/H]+0.16±0.01[8] dex
Rotational velocity (v sin i)1.9[7] km/s
Age6.0[10] or9.4±0.8[1] Gyr
79 Ceti B
Mass0.286[6] M
Radius0.361+0.004
−0.001
[3] R
Luminosity0.0132+0.009
−0.004
[3] L
Surface gravity (log g)4.84+0.02
−0.09
[3] cgs
Temperature3,265+3
−17
[3] K
Other designations
79 Cet,BD−04°426,FK5 4237,GJ 9085,HD 16141,HIP 12048,SAO 129992,WDS J02353-0334A,2MASS J02351994-0333376,Gaia DR2 2495335115182966016[11]
Database references
SIMBADdata
B

79 Ceti, also known asHD 16141, is abinary star system located 123 light-years from theSun in the southernconstellation ofCetus. It has anapparent visual magnitude of +6.83, which puts it below the normal limit for visibility with the average naked eye. The star is drifting closer to the Earth with a heliocentricradial velocity of −51 km/s.

Harlan (1974) assigned this star astellar classification of G2V,[5] matching an ordinaryG-type main-sequence star that is undergoingcorehydrogen fusion. However, Houk and Swift (1999) found a class of G8IV,[12] which suggests it has exhausted the supply ofhydrogen at its core and begun toevolve off the main sequence. Eventually the outer layers of the star will expand and cool and the star will become ared giant. Estimates of the star's age range from 6.0[10] to 9.4 billion years old.[1] It has an estimated 1.06 times themass of the Sun and 1.48 times theSun's radius.[9] The star is radiating twice[8]luminosity of the Sun from itsphotosphere at aneffective temperature of5,806 K.[8]

Ared dwarf companion at a projected separation of 220AU was discovered in 2005.[13] There is a suspicion that the companion may itself be a close binary.[4]

Planetary system

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On March 29, 2000, a planet orbiting primary star was announced, it was discovered using theradial velocity method.[14] This object has a minimum 0.26 times the mass ofJupiter and is orbiting its host star every 75.5 days.[15]

The 79 Ceti planetary system[16]
Companion
(in order from star)
MassSemimajor axis
(AU)
Orbital period
(days)
EccentricityInclinationRadius
b≥0.260±0.028 MJ0.363±0.02175.523±0.0550.252±0.052

See also

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References

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  1. ^abcdefgAnderson, 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. XHIP record for this object atVizieR.
  2. ^abcdefVallenari, A.; et al. (Gaia collaboration) (2023)."Gaia Data Release 3. Summary of the content and survey properties".Astronomy and Astrophysics.674: A1.arXiv:2208.00211.Bibcode:2023A&A...674A...1G.doi:10.1051/0004-6361/202243940.S2CID 244398875. Gaia DR3 record for this source atVizieR.
  3. ^abcdefghiVallenari, A.; et al. (Gaia collaboration) (2023)."Gaia Data Release 3. Summary of the content and survey properties".Astronomy and Astrophysics.674: A1.arXiv:2208.00211.Bibcode:2023A&A...674A...1G.doi:10.1051/0004-6361/202243940.S2CID 244398875. Gaia DR3 record for this source atVizieR.
  4. ^abTokovinin, Andrei (2018)."The Updated Multiple Star Catalog".The Astrophysical Journal Supplement Series.235 (1): 6.arXiv:1712.04750.Bibcode:2018ApJS..235....6T.doi:10.3847/1538-4365/aaa1a5.
  5. ^abHarlan, E. A. (June 1974). "MK classification for F- and G-type stars. III".Astronomical Journal.79:682–686.Bibcode:1974AJ.....79..682H.doi:10.1086/111597.
  6. ^abQuarles, Billy; Li, Gongjie; Kostov, Veselin; Haghighipour, Nader (2020)."Orbital Stability of Circumstellar Planets in Binary Systems".The Astronomical Journal.159 (3): 80.arXiv:1912.11019.Bibcode:2020AJ....159...80Q.doi:10.3847/1538-3881/ab64fa.S2CID 209444271.
  7. ^abcLindgren, Sara; Heiter, Ulrike; Seifahrt, Andreas (2016). "Metallicity determination of M dwarfs. High-resolution infrared spectroscopy".Astronomy and Astrophysics.586.arXiv:1510.06642.Bibcode:2016A&A...586A.100L.doi:10.1051/0004-6361/201526602.
  8. ^abcdefgS. G., Sousa; et al. (August 2008). "Spectroscopic parameters for 451 stars in the HARPS GTO planet search program. Stellar [Fe/H] and the frequency of exo-Neptunes".Astronomy and Astrophysics.487 (1):373–381.arXiv:0805.4826.Bibcode:2008A&A...487..373S.doi:10.1051/0004-6361:200809698.S2CID 18173201.
  9. ^abStassun, Keivan G.; et al. (March 2017)."Accurate Empirical Radii and Masses of Planets and Their Host Stars with Gaia Parallaxes".The Astronomical Journal.153 (3): 20.arXiv:1609.04389.Bibcode:2017AJ....153..136S.doi:10.3847/1538-3881/aa5df3.S2CID 119219062. 136.
  10. ^abSousa, S. G.; et al. (March 2010). "Higher depletion of lithium in planet host stars: no age and mass effect".Astronomy and Astrophysics.512: L5.arXiv:1003.0405.Bibcode:2010A&A...512L...5S.doi:10.1051/0004-6361/201014125.S2CID 118646949.
  11. ^"79 Cet".SIMBAD.Centre de données astronomiques de Strasbourg. Retrieved19 August 2017.
  12. ^Houk, N.; Swift, C. (1999). "Michigan catalogue of two-dimensional spectral types for the HD Stars".Michigan Spectral Survey.5.Bibcode:1999MSS...C05....0H.
  13. ^Mugrauer, M.; Neuhäuser, R.; Seifahrt, A.; Mazeh, T.; Guenther, E. (2005). "Four new wide binaries among exoplanet host stars".Astronomy and Astrophysics.440 (3): 1051.arXiv:astro-ph/0507101.Bibcode:2005A&A...440.1051M.doi:10.1051/0004-6361:20042297.
  14. ^"Keck astronomers discover planets smaller than saturn" (Press release). Kamuela, Hawaii: W. M. Keck Observatory. March 29, 2000. RetrievedAugust 13, 2019.
  15. ^Marcy, Geoffrey W.; et al. (2000). "Sub-Saturn Planetary Candidates of HD 16141 and HD 46375".The Astrophysical Journal Letters.536 (1):L43–L46.arXiv:astro-ph/0004326.Bibcode:2000ApJ...536L..43M.doi:10.1086/312723.PMID 10849416.S2CID 119530785.
  16. ^Butler, J. T.; et al. (2006). "Catalog of Nearby Exoplanets".The Astrophysical Journal.646 (1):505–522.arXiv:astro-ph/0607493.Bibcode:2006ApJ...646..505B.doi:10.1086/504701.S2CID 119067572.

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