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In 1921, Joel Stebbins announced that observations from 1917 through 1921 had shown that the star is an eclipsing binary. [14] AR Cassiopeiae A is an Algol-type eclipsing binary with an orbital period of about 6.07 days. [4] Its primary is a B-type main-sequence star, and the secondary an A-type main-sequence star. The secondary star may be an ...
In January 2006, NASA released images from the Hubble telescope, directly showing all three members of the Polaris ternary system. The nearer dwarf star is in an orbit of only 18.5 AU (2.8 billion km; about the distance from our Sun to Uranus ) from Polaris A, explaining why its light is swamped by its close and much brighter companion.
Nearest F-type main sequence star with a multiplanetary system. Second-brightest star in the night sky with a multiplanetary system after 7 Canis Majoris. All exoplanets orbit around star A in the binary system. 47 Ursae Majoris: Ursa Major: 10 h 59 m 27.97 s +40° 25′ 48.9″ 5.10: 46: G0V: 1.029: 5892: 7.434: 3
This category contains articles about star systems, which are groups of two or more gravitationally-bound stars in a region usually smaller than one light-year. Star clusters (groups of many more stars that occupy a much larger region) are listed in Category:Star clusters.
The star Polaris, often called either the "Pole Star" or the "North Star", is treated specially due to its proximity to the north celestial pole. When navigating in the Northern Hemisphere , a simple and quick technique can be used with Polaris to determine the observers latitude or, for larger maritime vessels can be used to calculate any ...
Polaris is a star in the northern circumpolar constellation of Ursa Minor. It is designated α Ursae Minoris (Latinized to Alpha Ursae Minoris) and is commonly called the North Star or Pole Star. With an apparent magnitude that fluctuates around 1.98, [3] it is the brightest star in the constellation and is readily visible to the naked eye at ...
TIC 168789840, also known as TYC 7037-89-1, [5] is a stellar system with six stars. [6] [4] Three pairs of binary stars circle a common barycenter.While other systems with three pairs of stars have been discovered, this was the first system where the stars can be observed eclipsing one another, as the Earth lies approximately on their planes of rotation.
In 2016, the International Astronomical Union (IAU) organized a Working Group on Star Names (WGSN) [2] to catalog and standardize proper names for stars. The WGSN's first bulletin, dated July 2016, [3] included a table of 125 stars comprising the first two batches of names approved by the WGSN (on 30 June and 20 July 2016) together with names of stars adopted by the IAU Executive Committee ...