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Epoch J2000 Equinox J2000
|Right ascension||15h 24m 29.4278s|
|Declination||+37° 22′ 37.8″|
|Apparent magnitude (V)||4.31 / 6.5|
|Spectral type||F0V + G1V|
|U−B color index||0.07 / 0.13|
|B−V color index||0.31 / 0.59|
|R−I color index||0.15 /|
|Radial velocity (Rv)||-12.5 km/s|
|Proper motion (μ)||RA: -147.68 mas/yr
Dec.: 84.69 mas/yr
|Parallax (π)||26.96 ± 0.65 mas|
|Distance||121 ± 3 ly
(37.1 ± 0.9 pc)
|Mu Boötis A|
|Surface gravity (log g)||4.14 cgs|
|Temperature||7,190 ± 140 K|
|Companion||CCDM 15245+3722 C|
|Period (P)||260.1 yr|
|Semi-major axis (a)||1.463"|
|Longitude of the node (Ω)||174.9°|
|Periastron epoch (T)||1865|
Bright Star Catalogue (5th rev. ed.)
Mu Boötis (μ Boötis, abbreviated Mu Boo, μ Boo) is a triple star system in the constellation of Boötes. The primary is designated μ¹ Boötis and the secondary (itself a binary star), μ² Boötis. Mu Boötis had the traditional name Alkalurops, although the International Astronomical Union now regards that name as only applying to μ¹ Boötis.
The system's traditional name Alkalurops is from the Greek καλαύροψ kalaurops "a herdsman's crook or staff", with the Arabic prefix attached. It has also been known as Inkalunis (from the Alfonsine tables), Clava (Latin 'the club') and Venabulum (Latin 'a hunting spear').
In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN) to catalogue and standardize proper names for stars. The WGSN approved the name Alkalurops for μ¹ Boötis on 21 August 2016 and it is now so entered in the IAU Catalog of Star Names.
It is known as 七公六, Qī Gōng liù (the Sixth Star of the Seven Excellencies) in Chinese.
μ¹ Boötis is a yellow-white F-type subgiant with an apparent magnitude of +4.31. Separated from the primary by 108 arcseconds in the sky is the binary star μ² Boötis, which has a combined spectral type of G1V and a combined brightness of +6.51 magnitudes. The components of μ² Boötis have apparent magnitudes of +7.2 and +7.8 and are separated by 2.2 arcseconds. They complete one orbit about their common centre of mass every 260 years.
- Malagnini, M. L.; Morossi, C. (November 1990), "Accurate absolute luminosities, effective temperatures, radii, masses and surface gravities for a selected sample of field stars", Astronomy and Astrophysics Supplement Series, 85 (3): 1015–1019, Bibcode:1990A&AS...85.1015M
- "IAU Catalog of Star Names". Retrieved 28 July 2016.
- Allen, Richard H. (1963). Star Names: Their Lore and Meaning (Reprint ed.). New York: Dover Publications Inc. p. 97. ISBN 0-486-21079-0. Retrieved 2016-09-15.
- Allen, Richard H. (1963). Star Names: Their Lore and Meaning (Reprint ed.). New York: Dover Publications Inc. p. 105. ISBN 0-486-21079-0. Retrieved 2016-09-15.
- IAU Working Group on Star Names (WGSN), International Astronomical Union, retrieved 22 May 2016.
- (Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 6 月 26 日