Editing Visual binary (section)

[[File:Theta1-Orionis-C.png | thumb | right | An example of a visual binary: Theta1 Orionis C1 (lower) and C2 (upper), as imaged by [[VLT/GRAVITY]].]]A '''visual binary''' is a gravitationally bound [[binary star]] system<ref>{{citation
 | first1=R. W. | last1=Argyle
 | title=Observing and Measuring Visual Double Stars
 | series=The Patrick Moore Practical Astronomy Series
 | publisher=Springer Science & Business Media
 | pages=71–75 | isbn=978-1461439455 | year=2012
 | url=https://books.google.com/books?id=DR9j2PODQOwC&pg=PA71
}}</ref> that can be resolved into two stars. These stars are estimated, via [[Johannes Kepler|Kepler]]'s [[Kepler's laws of planetary motion#Third_law|third law]], to have periods ranging from a few years to thousands of years. A visual binary consists of two stars, usually of a different brightness. Because of this, the brighter star is called the primary and the fainter one is called the companion. If the primary is too bright, relative to the companion, this can cause a glare making it difficult to resolve the two components.<ref>''The Binary Stars'', [[Robert Grant Aitken]], New York: Dover, 1964, p. 41.</ref> However, it is possible to resolve the system if observations of the brighter star show it to wobble about a centre of mass.<ref>{{cite web
 |url          = http://www.physics.utah.edu/~springer/phys3060/Lectures_files/lec10_2013.pdf
 |title        = Binary Systems and Stellar Parameters
 |access-date   = 2013-11-02
 |archive-url  = https://web.archive.org/web/20131104092847/http://www.physics.utah.edu/~springer/phys3060/Lectures_files/lec10_2013.pdf
 |archive-date = 2013-11-04
 |url-status     = dead
}}</ref> In general, a visual binary can be resolved into two stars with a telescope if their centres are separated by a value greater than or equal to one arcsecond, but with modern professional telescopes, interferometry, or space-based equipment, stars can be resolved at closer distances.

For a visual binary system, measurements taken need to specify, in arc-seconds, the apparent angular separation on the sky and the position angle{{snd}} which is the angle measured eastward from North in degrees{{snd}} of the companion star relative to the primary star. Taken over a period of time, the apparent relative orbit of the visual binary system will appear on the celestial sphere. The study of visual binaries reveals useful stellar characteristics: masses, densities, surface temperatures, luminosity, and rotation rates.<ref name="Binary">{{cite book
 | author = Michael Zeilik
 | author2 = Stephan A. Gregory
 | author3 = Elske V. P. Smith | author3-link = Elske Smith
 | name-list-style = amp  
 | title = Introductory Astronomy and Astrophysics 
 | year = 1998
 | isbn = 978-0030062285 
 | publisher = Brooks/Cole 
}}</ref>