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#REDIRECT [[Common envelope]] [[Category:Binary stars|*]] ...

{{Short description|Binary star system whose component stars are very close}} {{About|contact binary stars|comets and minor planets|Contact binary (small Solar System body)}} ...

| notes = A peculiar PN with a binary in the center ...2=Reay |first2=N. K. |date=1983 |title=Ansae and the precession of central stars in planetary nebulae - The cases of NGC 5189 and NGC 6826 |journal=Astronom ...

...thumb|Schematic of a W Ursae Majoris variable with a mass ratio of 3. Both stars (the filled regions) overfill their Roche lobes (enclosed by the black line ...rphology and the Name Overcontact|journal=Information Bulletin on Variable Stars|volume=5076 |pages=1|bibcode=2001IBVS.5076....1W}}</ref> ...

...el Waisberg ''et al''. This inner system will become a [[common envelope]] binary, when 58 Aquarii Aa expands in the [[red giant]] phase. Mass transfer betwe .... XI. Uncovering a {{solar mass|0.7}}, 2.3 au Companion in the Astrometric Binary HIP 111200 = 58 Aquarii |bibcode=2023RNAAS...7..225W |journal=Research Note ...

...acteristics is its unusually cool central star, which is a [[spectroscopic binary]], and its unusual shape. ...a is the result of [[ultraviolet astronomy|ultraviolet]] emission from the binary companion.<ref name=Phillips2000/> The stronger infrared emission from mole ...

...[[bright giant]]). In the standard [[Hertzsprung–Russell diagram]], these stars lie above and to the right of the [[main sequence]]. ...[red giant]]s, because they only develop from more massive and less common stars, and because they have short lives in the blue giant stage. ...

{{Short description|Binary star system in the constellation Sculptor}} ...red spectroscopic detection of the brown dwarf in the post common envelope binary WD 0137-349|journal=Monthly Notices of the Royal Astronomical Society: Lett ...

{{Short description|Gravitationally-binding region around a star in a binary system}} ...configuration q=3.svg|right|thumb|This is a schematic of a [[semidetached binary]] system with the larger component filling its Roche lobe (black line).]] ...

{{short description|Highly magnetic type of cataclysmic variable binary star system}} ...its [[Roche lobe]].<ref name=":0">{{Cite book|title = Cataclysmic Variable Stars|last = Hellier|first = Coel|publisher = Springer|year = 2001}}</ref> Polar ...

{{short description|Binary star in the constellation Aquarius}} ...ry/optical-IR-prod/wds/orb6|title=Sixth Catalog of Orbits of Visual Binary Stars|publisher=United States Naval Observatory|access-date=3 June 2017|archive-d ...

...R Lyrae stars in green, and some of the more luminous [[red-giant branch]] stars in red ...in [[Luminosity#In astronomy|luminosity]], some contraction of the stellar envelope, and the surface reaching higher temperatures. ...

...sual magnitude]] of +3.37 at its brightest, making it one of the [[List of stars in Taurus|brighter members]] of the constellation. Based upon [[parallax]] ...ude.<ref name=aaa42_2_229/> The mean physical separation between these two stars is estimated at 21.91 times the radius of the Sun, or {{val|0.1|ul=Astronom ...

{{Short description|Nuclear fusion type found in older stars}} ...means higher temperatures, although lower densities, than for less massive stars.<ref name="Clayton">{{cite book|last=Clayton|first=Donald| url=https://arch ...

...ium''' ("Engraver's Chisel"); it is a rare word, unrelated to the far more common Latin ''caelum'', meaning "[[sky]]", "[[heaven]]", or "[[atmosphere]]".<ref .../sub>. Other notable objects in Caelum are [[RR Caeli|RR&nbsp;Caeli]], a [[binary star]] with one known planet approximately {{convert|20.13|pc|ly}} away; [[ ...

...e web | url=https://www.iau.org/public/themes/naming_stars/ | title=Naming Stars |publisher=IAU.org |access-date=16 December 2017}}</ref> is a [[star]] in t ...ccess-date=22 May 2016}}</ref> to catalog and standardize proper names for stars. The WGSN approved the name ''Alzirr'' for this star on 30 June 2017 and it ...

...rbon monoxide]] (CO) molecules produced after stellar co-absorption in a [[binary system]] of the nebula which outflow as a [[Cosmic wind|gas wind]] were les ...in the outer environment (an envelope) of the dual orbital system of the binary system.<ref name=Ivanovaetal0159-013-0059-2/> The KE within the outflow is ...

'''Lambda Aquilae''' is a [[binary star]] in the [[constellation]] [[Aquila (constellation)|Aquila]]. Its iden ...ndary. Before this, there was evidence for a companion via [[spectroscopic binary|spectroscopy]] and [[adaptive optics]], but a sequence of detections and no ...

...iated at an [[effective temperature]] of over 22,000&nbsp;K from the outer envelope, giving it the blue-white hue of a [[B-type star]].<ref name=csiro/> It has ...ion|OB association]], the nearest such of association of co-moving massive stars to the Sun.<ref name=aaa216_1_44/> ...

...[[Bright Star Catalogue|HR]]&nbsp;7194, [[Index Catalogue of Visual Double Stars|IDS]]&nbsp;18562-3001 AB, [[PPM Star Catalogue|PPM]]&nbsp;269230, [[Smithso ...names for stars. The WGSN decided to attribute proper names to individual stars rather than entire [[multiple star|multiple systems]].<ref name="TriRpt18" ...