Editing Boötes (section)

==== Multiple stars ====
<!-- Deleted image removed: [[File:Celestial photograph of Bootes.jpg|500px|thumbnail|left|Celestial photograph depicting many of Boötes' double and multiple stars. Arcturus is the bright white star in the lower right. The semicircle of stars near the bottom left is the neighboring constellation Corona Borealis.]] -->
Besides Pulcherrima and Alkalurops, there are several other binary stars in Boötes:
 
*[[Xi Boötis]] is a quadruple star popular with amateur astronomers. The primary is a yellow star of magnitude 4.7 and the secondary is an orange star of magnitude 6.8. The system is 22 light-years away and has an orbital period of 150 years.{{sfn|Ridpath|2001|pp=88–89}} The primary and secondary have a separation of 6.7 arcseconds at an angle of 319 degrees.{{sfn|Moore|2000|pp=341–342}} The tertiary is a magnitude 12.6 star (though it may be observed to be brighter) and the quaternary is a magnitude 13.6 star.{{sfn|Thompson|Thompson|2007|p=105}} 
* [[Pi Boötis]] is a close triple star. The primary is a blue-white star of magnitude 4.9, the secondary is a blue-white star of magnitude 5.8,{{sfn|Ridpath|2001|pp=88–89}} and the tertiary is a star of magnitude 10.4.{{sfn|Thompson|Thompson|2007|p=105}} The primary and secondary components are separated by 5.6 arcseconds at an angle of 108 degrees;{{sfn|Moore|2000|pp=341–342}} the primary and tertiary components are separated by 128 arcseconds at an angle of 128 degrees.{{sfn|Thompson|Thompson|2007|p=105}}
* [[Zeta Boötis]] is a triple star that consists of a [[binary star|physical binary]] pair with an [[double star|optical]] companion. Lying 205 light-years away from Earth, The physical pair has a period of 123.3 years and consists of a magnitude 4.5 and a magnitude 4.6 star. The two components are separated by 1.0 arcseconds at an angle of 303 degrees. The optical companion is of magnitude 10.9, separated by 99.3 arcseconds at an angle of 259 degrees. [[44 Boötis]] is an eclipsing variable star. The primary is of variable magnitude and the secondary is of magnitude 6.2; they have an orbital period of 225 years. The components are separated by 1.0 arcsecond at an angle of 40 degrees.{{sfn|Moore|2000|pp=341–342}}

44 Boötis (i Boötis) is a double variable star 42 light-years away. It has an overall magnitude of 4.8 and appears yellow to the naked eye. The primary is of magnitude 5.3 and the secondary is of magnitude 6.1; their orbital period is 220 years. The secondary is itself an eclipsing variable star with a range of 0.6 magnitudes; its orbital period is 6.4 hours.{{sfn|Ridpath|2001|pp=88–89}} It is a [[W Ursae Majoris variable]] that ranges in magnitude from a minimum of 7.1 to a maximum of 6.5 every 0.27 days. Both stars are G-type stars. Another eclipsing binary star is [[ZZ Boötis]], which has two F2-type components of almost equal mass,{{sfn|Popper 1983}} and ranges in magnitude from a minimum of 6.79 to a maximum of 7.44 over a period of 5.0 days.{{sfn|AAVSO ZZ Boötis}}