Epsilon Boötis (ε Boötis, abbreviated Epsilon Boo, ε Boo), officially named Izar,[1] is a binary star in the northern constellation of Boötes. The star system can be viewed with the unaided eye at night, but resolving the pair with a small telescope is challenging; an aperture of 76mm or greater is required.
ε Boötis (Latinised to Epsilon Boötis) is the star's Bayer designation.
It bore the traditional names Izar, Mirak and Mizar, and was named Latin: Pulcherrima by Friedrich Georg Wilhelm von Struve.[2] Izar, and Mizar are from the Arabic: إزار|rtl=yes Arabic: ʾizār and مئزر Mi'zar ('kilt like undergarment') and Arabic: المراق|rtl=yes Arabic: al-maraqq' ('the loins'); Latin: Pulcherrima is Latin for 'loveliest'. In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN)[3] to catalogue and standardize proper names for stars. The WGSN approved the name Izar for this star on 21 August 2016 and it is now so entered in the IAU Catalog of Star Names.[1]
In the catalogue of stars in the Calendarium of Al Achsasi Al Mouakket, this star was designated Arabic: Mintek al Aoua (Arabic: منطقة العوّاء|rtl=yes Arabic: minṭáqa al awwa), which was translated into Latin as Latin: Cingulum Latratoris, meaning 'belt of barker'.In Chinese astronomy, Chinese: 梗河 Chinese: Gěng Hé ('Celestial Lance'), refers to an asterism consisting of Epsilon Boötis, Sigma Boötis and Rho Boötis.[4] Consequently, the Chinese name for Epsilon Boötis itself is Chinese: 梗河一 Chinese: Gěng Hé yī ('the First Star of Celestial Lance').[5]
Epsilon Boötis consists of a pair of stars with an angular separation of at a position angle of . The brighter component (A) has an apparent visual magnitude of 2.37, making it readily visible to the naked eye at night. The fainter component (B) is at magnitude 5.12, which by itself would also be visible to the naked eye. Parallax measurements from the Hipparcos astrometry satellite put the system at a distance of about 203abbr=offNaNabbr=off from the Earth. This means the pair has a projected separation of 185 Astronomical Units, and they orbit each other with a period of at least 1,000 years.
The brighter member has a stellar classification of K0 II-III, which means it is a fairly late-stage star well into its stellar evolution, having already exhausted its supply of hydrogen fuel at the core. With more than four times the mass of the Sun, it has expanded to about 38 times the Sun's radius and is emitting 650 times the luminosity of the Sun. This energy is being radiated from its outer envelope at an effective temperature of 4,755 K, giving it the orange hue of a K-type star.
The companion star has a classification of A2 V, so it is a main sequence star that is generating energy through the thermonuclear fusion of hydrogen at its core. This star is rotating rapidly, with a projected rotational velocity of . It has a surface temperature of about and a radius nearly three times the Sun, leading to a bolometric luminosity 45 times that of the Sun.
By the time the smaller main sequence star reaches the current point of the primary in its evolution, the larger star will have lost much of its mass in a planetary nebula and will have evolved into a white dwarf. The pair will have essentially changed roles: the brighter star becoming the dim dwarf, while the lesser companion will shine as a giant star.
In 1973, the Scottish astronomer and science fiction writer Duncan Lunan claimed to have managed to interpret a message caught in the 1920s by two Norwegian physicists that, according to his theory, came from a 13,000 year old satellite polar orbiting the Earth known as the Black Knight and sent there by the inhabitants of a planet orbiting Epsilon Boötis.[6] The story was even reported in Time magazine. Lunan later withdrew his Epsilon Boötis theory, presenting proofs against it and clarifying why he was brought to formulate it in the first place, but later revoked his withdrawal.