Astronomy:Mu Ceti
  | |
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Cetus |
| Right ascension | 02h 44m 56.54098s[1] |
| Declination | 10° 06′ 50.9089″[1] |
| Apparent magnitude (V) | +4.27[2] |
| Characteristics | |
| Spectral type | A9IIIp[3] |
| Variable type | suspected δ Sct[4] |
| Astrometry | |
| Parallax (π) | 38.80 ± 0.32[1] mas |
| Distance | 84.1 ± 0.7 ly (25.8 ± 0.2 pc) |
| Absolute magnitude (MV) | +2.17[5] |
| Details | |
| Mass | 1.6[6] M☉ |
| Radius | 1.7[6] R☉ |
| Luminosity | 7.5[6] L☉ |
| Temperature | 7,141[5] K |
| Rotational velocity (v sin i) | 45.1±2.3[5] km/s |
| Age | 3.3[6] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Mu Ceti (μ Ceti) is a star in the constellation Cetus. The combined apparent magnitude of the system is +4.27, and it 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 1,202 days.[6] Later studies have failed to find any evidence of these companions.[10]
References
- ↑ 1.0 1.1 1.2 Van Leeuwen, F (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics 474 (2): 653–664. doi:10.1051/0004-6361:20078357. Bibcode: 2007A&A...474..653V.
- ↑ Samus, N. N. 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.
- ↑ 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. doi:10.1086/378365. Bibcode: 2003AJ....126.2048G.
- ↑ 4.0 4.1 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.
- ↑ 5.0 5.1 5.2 Reiners, Ansgar (January 2006), "Rotation- and temperature-dependence of stellar latitudinal differential rotation", Astronomy and Astrophysics 446 (1): 267–277, doi:10.1051/0004-6361:20053911, Bibcode: 2006A&A...446..267R
- ↑ 6.0 6.1 6.2 6.3 6.4 Jim Kaler (Dec 21, 2007). "Mu Ceti". http://stars.astro.illinois.edu/sow/mucet.html.
- ↑ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 11 日
- ↑ 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. doi:10.1086/190199. Bibcode: 1969ApJS...19...79B.
- ↑ Adelman, S. J (2001). "Research Note Hipparcos photometry: The least variable stars". Astronomy and Astrophysics 367: 297–298. doi:10.1051/0004-6361:20000567. Bibcode: 2001A&A...367..297A.
- ↑ 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 (1): 4. doi:10.3847/0067-0049/227/1/4. Bibcode: 2016ApJS..227....4H.
 |  |
