Mu Ceti

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μ Ceti
Cetus constellation map.svg
Red circle.svg
Location of μ Ceti (circled)
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Cetus
Right ascension  02h 44m 56.54098s[1]
Declination 10° 06′ 50.9089″[1]
Apparent magnitude (V) +4.27[2]
Spectral type A9IIIp[3]
Variable type suspected δ Sct[4]
Parallax (π)38.80 ± 0.32[1] mas
Distance84.1 ± 0.7 ly
(25.8 ± 0.2 pc)
Absolute magnitude (MV)+2.17[5]
Mass1.6[6] M
Radius1.7[6] R
Luminosity7.5[6] L
Temperature7,141[5] K
Rotational velocity (v sin i)45.1±2.3[5] km/s
Age3.3[6] Gyr
Other designations
87 Ceti, HD 17094, HIP 12828, HR 813, SAO 110723, BD+09° 359
Database references

Mu Ceti (μ Ceti) is a star in the constellation Cetus. The combined apparent magnitude of the system is +4.27, and is located 84 light years from the Sun.

In Chinese, 天囷 (Tiān Qūn), meaning Circular Celestial Granary, refers to an asterism consisting of α Ceti, κ1 Ceti, λ Ceti, μ Ceti, ξ1 Ceti, ξ2 Ceti, ν Ceti, γ Ceti, δ Ceti, 75 Ceti, 70 Ceti, 63 Ceti and 66 Ceti. Consequently, the Chinese name for Mu Ceti itself is "the Fourth Star of Circular Celestial Granary".[7]

Mu Ceti is an A9 giant star. It has been suspected to be a δ Scuti variable,[4] but most studies find it to be of constant brightness.[8][9]

Three companions were all discovered during occultations of Mu Ceti by the Moon. An orbit was derived for the brightest with a period of 1202 days.[6] Later studies have failed to find any evidence of these companions.[10]


  1. ^ a b c Van Leeuwen, F (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357.
  2. ^ Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/gcvs. Originally published in: 2009yCat....102025S. 1. Bibcode:2009yCat....102025S.
  3. ^ Gray, R. O; Corbally, C. J; Garrison, R. F; McFadden, M. T; Robinson, P. E (2003). "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 Parsecs: The Northern Sample. I". The Astronomical Journal. 126 (4): 2048. arXiv:astro-ph/0308182. Bibcode:2003AJ....126.2048G. doi:10.1086/378365.
  4. ^ a b Hauck, B (1971). "Short period variable stars. V. Delta Scuti-type stars in the Geneva system". Astronomy and Astrophysics. 11: 79. Bibcode:1971A&A....11...79H.
  5. ^ a b c Reiners, A. (January 2006), "Rotation- and temperature-dependence of stellar latitudinal differential rotation", Astronomy and Astrophysics, 446 (1): 267–277, arXiv:astro-ph/0509399, Bibcode:2006A&A...446..267R, doi:10.1051/0004-6361:20053911.
  6. ^ a b c d e Jim Kaler (Dec 21, 2007). "Mu Ceti".
  7. ^ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 11 日
  8. ^ Breger, Michel (1969). "Short-Period Variability of b, a, and F Stars. III. A Survey of Delta Scuti Variable Stars". Astrophysical Journal Supplement. 19: 79. Bibcode:1969ApJS...19...79B. doi:10.1086/190199.
  9. ^ Adelman, S. J (2001). "Research Note Hipparcos photometry: The least variable stars". Astronomy and Astrophysics. 367: 297. Bibcode:2001A&A...367..297A. doi:10.1051/0004-6361:20000567.
  10. ^ Hutter, D. J; Zavala, R. T; Tycner, C; Benson, J. A; Hummel, C. A; Sanborn, J; Franz, O. G; Johnston, K. J (2016). "Surveying the Bright Stars by Optical Interferometry. I. A Search for Multiplicity among Stars of Spectral Types F-K". The Astrophysical Journal Supplement Series. 227: 4. arXiv:1609.05254. Bibcode:2016ApJS..227....4H. doi:10.3847/0067-0049/227/1/4.