79 Ceti

79 Ceti
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Cetus
Right ascension 02h 35m 19.9293s[1]
Declination −03° 33′ 38.1707″[1]
Apparent magnitude (V) +6.83[2]
Characteristics
Spectral type G2V+M[3][4] or G8IV[5]
B−V color index 0.670±0.004[2]
Variable type none
Astrometry
Radial velocity (Rv)−50.93±0.09[2] km/s
Proper motion (μ) RA: −155.58[1] mas/yr
Dec.: −437.99[1] mas/yr
Parallax (π)26.4360 ± 0.0580 mas[1]
Distance123.4 ± 0.3 ly
(37.83 ± 0.08 pc)
Absolute magnitude (MV)+3.88[2]
Details[6]
79 Ceti A
Mass1.01 M☉
Radius1.48[7] R☉
Luminosity1.99±0.04 L☉
Surface gravity (log g)4.19±0.02 cgs
Temperature5,806±17 K
Metallicity [Fe/H]+0.16±0.01[6] dex
Age6.0[8] or 9.4±0.8[2] Gyr
79 Ceti B
Mass0.286[4] M☉
Other designations
79 Cet, BD−04°426, FK5 4237, Gaia DR2 2495335115182966016, GJ 9085, HD 16141, HIP 12048, SAO 129992, WDS J02353-0334A, 2MASS J02351994-0333376[9]
Database references
SIMBADdata

79 Ceti, also known as HD 16141, is a binary star system located 123[1] light-years from the Sun in the southern constellation of Cetus. It has an apparent visual magnitude of +6.83,[2] which puts it below the normal limit for visibility with the average naked eye. The star is drifting closer to the Earth with a heliocentric radial velocity of −51 km/s.[2]

Harlan (1974) assigned this star a stellar classification of G2V,[3] matching an ordinary G-type main-sequence star that is undergoing core hydrogen fusion. However, Houk and Swift (1999) found a class of G8IV,[5] which suggests it has exhausted the supply of hydrogen at its core and begun to evolve off the main sequence. Eventually the outer layers of the star will expand and cool and the star will become a red giant. Estimates of the star's age range from 6.0[8] to 9.4 billion years old. It has an estimated 1.06 times the mass of the Sun and 1.48[7] times the Sun's radius. The star is radiating twice[6] luminosity of the Sun from its photosphere at an effective temperature of 5,806 K.[6] The discrepancy was later found to be due to an additional red dwarf star in the system at a projected separation 220 AUs.[4]

  1. ^ a b c d e f Cite error: The named reference Gaia DR2 was invoked but never defined (see the help page).
  2. ^ a b c d e f g Cite error: The named reference Anderson2012 was invoked but never defined (see the help page).
  3. ^ a b Cite error: The named reference Harlan1974 was invoked but never defined (see the help page).
  4. ^ a b c Quarles, 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
  5. ^ a b Cite error: The named reference Houk1999 was invoked but never defined (see the help page).
  6. ^ a b c d Cite error: The named reference Sousa2008 was invoked but never defined (see the help page).
  7. ^ a b Cite error: The named reference Stassun2017 was invoked but never defined (see the help page).
  8. ^ a b Cite error: The named reference aaa512_L5 was invoked but never defined (see the help page).
  9. ^ Cite error: The named reference SIMBAD was invoked but never defined (see the help page).