Epsilon Ursae Majoris
Epsilon Ursae Majoris (Latinised from ε Ursae Majoris, abbreviated Epsilon UMa, ε UMa), officially named Alioth //, is, despite being designated "ε" (epsilon), the brightest star in the constellation of Ursa Major, and at magnitude 1.77 is the thirty-second brightest star in the sky.
Epoch J2000 Equinox J2000
|Right ascension||12h 54m 01.74959s|
|Declination||+55° 57′ 35.3627″|
|Apparent magnitude (V)||1.77|
|Spectral type||A1III-IVp kB9|
|U−B color index||+0.02|
|B−V color index||-0.02|
|Variable type||α2 CVn|
|Radial velocity (Rv)||-9.3 km/s|
|Proper motion (μ)|| RA: +111.91 mas/yr |
Dec.: -8.24 mas/yr
|Parallax (π)||39.51 ± 0.20 mas|
|Distance||82.6 ± 0.4 ly |
(25.3 ± 0.1 pc)
|Absolute magnitude (MV)||–0.2|
|Surface gravity (log g)||3.23 cgs|
|Metallicity [Fe/H]||+0.00 dex|
|Rotational velocity (v sin i)||33 km/s|
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 (or 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.
According to Hipparcos, Epsilon Ursae Majoris is 81 light-years (25 parsecs) from the Sun. Its spectral type is A1p; the "p" stands for peculiar, as its spectrum is characteristic of an α2 Canum Venaticorum variable. Epsilon Ursae Majoris, 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 Epsilon Ursae Majoris and the Earth. The intervening elements react differently at different frequencies of light as they whip in and out of view, causing Epsilon Ursae Majoris 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.
Epsilon Ursae Majoris's rotational and magnetic poles are at almost 90 degrees to one another. Darker (denser) regions of chromium form a band at right angles to the equator.
It has long been suspected that Epsilon Ursae Majoris is a spectroscopic binary, possibly with more than one companion. A more recent study suggests Epsilon Ursae Majoris'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. It is now thought that the 5.1-day period is the rotation period of the star, and no companions have been detected using the most modern equipment.
Name and etymologyEdit
The traditional name Alioth comes from the Arabic alyat al-hamal ("the sheep's fat tail"). In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN) to catalog and standardize proper names for stars. The WGSN's first bulletin of July 2016 included a table of the first two batches of names approved by the WGSN; which included Alioth for this star.
In Chinese, 北斗 (Běi Dǒu), meaning Northern Dipper, refers to an asterism equivalent to the Big Dipper. Consequently, the Chinese name for Epsilon Ursae Majoris itself is 北斗五 (Běi Dǒu wu, English: the Fifth Star of Northern Dipper) and 玉衡 (Yù Héng, English: Star of Jade Sighting-Tube).
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