Epsilon Ursae Majoris
  Alioth in Ursa Major (circled). | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Ursa Major |
| Right ascension | 12h 54m 01.74959s[1] |
| Declination | +55° 57′ 35.3627″[1] |
| Apparent magnitude (V) | 1.77[2] |
| Characteristics | |
| Spectral type | A1III-IVp kB9 |
| U−B color index | +0.02[2] |
| B−V color index | -0.02[2] |
| Variable type | α2-CVn |
| Astrometry | |
| Radial velocity (Rv) | -9.3[3] km/s |
| Proper motion (μ) | RA: +111.91[1] mas/yr Dec.: -8.24[1] mas/yr |
| Parallax (π) | 39.51 ± 0.20[1] mas |
| Distance | 82.6 ± 0.4 ly (25.3 ± 0.1 pc) |
| Absolute magnitude (MV) | –0.2[4] |
| Details | |
| Mass | 2.91[5] M☉ |
| Radius | 4.2 ± 0.2[6] R☉ |
| Luminosity | 108 L☉ |
| Surface gravity (log g) | 3.5[4] cgs |
| Temperature | 10,800[4] K |
| Metallicity [Fe/H] | +0.00[4] dex |
| Rotational velocity (v sin i) | 33[7] km/s |
| Other designations | |
| Database references | |
| SIMBAD | data |
Epsilon Ursae Majoris (Epsilon UMa, ε Ursae Majoris, ε UMa) is the brightest star in the constellation Ursa Major (despite its Bayer designation being merely "epsilon"), and at magnitude 1.76 is the thirty-first brightest star in the sky. It has the traditional name Alioth. It is the star in the tail of the bear closest to its body, and thus the star in the handle of the Big Dipper (Plough) closest to the bowl. It is also a member of the large and diffuse Ursa Major moving group. Historically, the star was frequently used in celestial navigation in the maritime trade, because it is listed as one of the 57 navigational stars.[1]
Peculiarities
According to Hipparcos, Alioth is 81 light years (25 parsecs) from Earth. Its spectral type is A1p; the "p" stands for peculiar, as the spectrum of its light is characteristic of an Alpha2 Canum Venaticorum variable. Alioth, as a representative of this type, may harbor two interacting processes. First, the star's strong magnetic field separating different elements in the star's hydrogen 'fuel'. In addition, a rotation axis at an angle to the magnetic axis may be spinning different bands of magnetically sorted elements into the line of sight between Alioth and the Earth. The intervening elements react differently at different frequencies of light as they whip in and out of view, causing Alioth to have very strange spectral lines that fluctuate over a period of 5.1 days. The kB9 suffix to the spectral type indicates that the calcium K line is present and representative of a B9 spectral type even though the rest of the spectrum indicates A1.
With Alioth, the rotational and magnetic axes are at almost 90 degrees to one another. Darker (denser) regions of chromium form a band at right angles to the equator.
A recent study suggests Alioth's 5.1-day variation may be due to a substellar object of about 14.7 Jupiter masses in an eccentric orbit (e=0.5) with an average separation of 0.055 astronomical units.
Alioth has a relatively weak magnetic field, 15 times weaker than α CVn, but it is still 100 times stronger than that of the Earth.
Name and etymology
- The traditional name Alioth comes from the Arabic alyat (fat tail of a sheep).
- This star as Añgiras, one of the Seven Rishis.[8]
- In Chinese, 北斗 (Běi Dǒu), meaning Northern Dipper, refers to an asterism consisting of ε Ursae Majoris, α Ursae Majoris, β Ursae Majoris, γ Ursae Majoris, δ Ursae Majoris, ζ Ursae Majoris and η Ursae Majoris. Consequently, ε Ursae Majoris itself is known as 北斗五 (Běi Dǒu wu, English: the Fifth Star of Northern Dipper) and 玉衡 (Yù Héng, English: Star of Jade Sighting-Tube).[9]
Namesakes
USS Allioth (AK-109) was a United States Navy Crater class cargo ship named after the star.
See also
References
- 1 2 3 4 5 van Leeuwen, F. (November 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
- 1 2 3 Johnson, H. L.; et al. (1966). "UBVRIJKL photometry of the bright stars". Communications of the Lunar and Planetary Laboratory 4 (99): 99. Bibcode:1966CoLPL...4...99J.
- ↑ Evans, D. S. (June 20–24, 1966), Batten, Alan Henry; Heard, John Frederick, eds., "The Revision of the General Catalogue of Radial Velocities", Determination of Radial Velocities and their Applications (University of Toronto: International Astronomical Union) 30: 57, Bibcode:1967IAUS...30...57E
- 1 2 3 4 Tektunali, H. G. (June 1981), "The spectrum of the CR star Epsilon Ursae Majoris", Astrophysics and Space Science 77 (1): 41–58, Bibcode:1981Ap&SS..77...41T, doi:10.1007/BF00648756
- ↑ Shaya, Ed J.; Olling, Rob P. (January 2011), "Very Wide Binaries and Other Comoving Stellar Companions: A Bayesian Analysis of the Hipparcos Catalogue", The Astrophysical Journal Supplement 192 (1): 2, arXiv:1007.0425, Bibcode:2011ApJS..192....2S, doi:10.1088/0067-0049/192/1/2
- ↑ Sokolov, N. A. (March 2008), "Radial velocity study of the chemically peculiar star ɛ Ursae Majoris", Monthly Notices of the Royal Astronomical Society: Letters 385 (1): L1–L4, arXiv:0904.3562, Bibcode:2008MNRAS.385L...1S, doi:10.1111/j.1745-3933.2008.00419.x.
- ↑ Royer, F.; et al. (October 2002), "Rotational velocities of A-type stars in the northern hemisphere. II. Measurement of v sin i", Astronomy and Astrophysics 393 (3): 897–911, arXiv:astro-ph/0205255, Bibcode:2002A&A...393..897R, doi:10.1051/0004-6361:20020943
- ↑ Allen, R. H. (1963). Star Names: Their Lore and Meaning (Reprint ed.). New York: Dover Publications Inc. p. 438. ISBN 0-486-21079-0. Retrieved 2012-09-04.
- ↑ (Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 6 月 15 日
- ^
This article incorporates text from a publication now in the public domain: Chambers, Ephraim, ed. (1728). "article name needed". Cyclopædia, or an Universal Dictionary of Arts and Sciences (first ed.). James and John Knapton, et al.
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