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• RS_Canum_Venaticorum_variable abstract "RS Canum Venaticorum variables are a type of variable star. They are close binary stars having active chromospheres which can cause large stellar spots. These spots are believed to cause variations in their observed luminosity. Systems can exhibit variations on timescales of years due to variation in the spot surface coverage fraction, as well as periodic variations which are, in general, close to the orbital period of the binary system. Some systems exhibit variations in luminosity due to their being eclipsing binaries. Typical brightness fluctuation is around 0.2 magnitudes.Struve (1946) first called attention to the group, but it was Oliver (1974) who was the first to formally propose a set of observational characteristics to define the RS CVn criteria. The working definition, as it is used today, was that set down by Hall (1976).The RS CVn systems are divided into five separate subgroups:I. Regular Systems:Orbital periods between 1 and 14 days.The hotter component is of the spectral type F or G and luminosity class V or IV.Strong Ca II H and K emission is seen outside of eclipse.II. Short Period Systems:Components are detached.Orbital periods less than 1 day.The hotter component is of the spectral type F or G and luminosity class V or IV.Ca II H and K emission is displayed in one or both components.III. Long Period Systems:Orbital periods greater than 14 days.Either component is of the spectral type G through K and luminosity class II through IV.Strong Ca II H and K emission is seen outside of eclipse.IV. Flare Star SystemsThe hotter component is of the spectral type dKe or dMe, where the emission refers to strong Ca II H and K.V. V471 Tau Type Systems:The hotter component is a white dwarf.The cooler component, spectral class G through K, displays strong Ca II H and K emission.The light curves of RS CVn type systems show a peculiar semiperiodic structure outside of eclipse. This structure has been referred to as a distortion wave in the light curve. Eaton and Hall (1979) determined that the simplest mechanism for the creation of the distortion wave was "starspots", which, in analogy to sunspots, are large, cool active regions on the photosphere. Such spots have since been observed indirectly on many systems.Chromospheric activity is signaled by the presence of emission cores in the Ca II H and K resonance lines. Balmer emission, or Hα, is also associated with active chromospheres. X-ray emission is known as a tracer for active coronal regions, and ultraviolet (UV) emission and flaring are, by solar analogy, known to be associated with stellar active and transition regions. These areas on the Sun are associated with intense magnetic fields, and sunspot activity is enhanced in and around these magnetically active regions.Some RS CVn's are known X-ray and radio emitters. The radio emission is nonthermal in origin (gyrosynchrotron) and is one of the few direct indicators of magnetic fields. The X-ray luminosities are on the order of Lx >> 1024 watts. This emission has been interpreted, in solar analogy, as being caused by a hot, T ~ 107 K, corona.Another subgroup of RS CVNs is known to have infrared excess emission, seen by the Spitzer Space Telescope".
• RS_Canum_Venaticorum_variable wikiPageExternalLink imaging.html.
• RS_Canum_Venaticorum_variable wikiPageExternalLink lrsp-2005-8.
• RS_Canum_Venaticorum_variable wikiPageID "2712404".
• RS_Canum_Venaticorum_variable wikiPageRevisionID "565663907".
• RS_Canum_Venaticorum_variable hasPhotoCollection RS_Canum_Venaticorum_variable.
• RS_Canum_Venaticorum_variable subject Category:Binary_stars.
• RS_Canum_Venaticorum_variable subject Category:RS_Canum_Venaticorum_variables.
• RS_Canum_Venaticorum_variable subject Category:Variable_stars.
• RS_Canum_Venaticorum_variable type BinaryStar109221070.
• RS_Canum_Venaticorum_variable type BinaryStars.
• RS_Canum_Venaticorum_variable type CelestialBody109239740.
• RS_Canum_Venaticorum_variable type NaturalObject100019128.
• RS_Canum_Venaticorum_variable type Object100002684.
• RS_Canum_Venaticorum_variable type PhysicalEntity100001930.
• RS_Canum_Venaticorum_variable type RSCanumVenaticorumVariables.
• RS_Canum_Venaticorum_variable type Star109444100.
• RS_Canum_Venaticorum_variable type Thing100002452.
• RS_Canum_Venaticorum_variable type Variable109468959.
• RS_Canum_Venaticorum_variable type VariableStar109469152.
• RS_Canum_Venaticorum_variable type VariableStars.
• RS_Canum_Venaticorum_variable type Whole100003553.
• RS_Canum_Venaticorum_variable comment "RS Canum Venaticorum variables are a type of variable star. They are close binary stars having active chromospheres which can cause large stellar spots. These spots are believed to cause variations in their observed luminosity. Systems can exhibit variations on timescales of years due to variation in the spot surface coverage fraction, as well as periodic variations which are, in general, close to the orbital period of the binary system.".
• RS_Canum_Venaticorum_variable label "Estrella variable RS Canum Venaticorum".
• RS_Canum_Venaticorum_variable label "Gwiazdy typu RS Canum Venaticorum".
• RS_Canum_Venaticorum_variable label "RS Canum Venaticorum variable".
• RS_Canum_Venaticorum_variable label "RS-Canum-Venaticorum-Stern".
• RS_Canum_Venaticorum_variable label "Variabile RS Canum Venaticorum".
• RS_Canum_Venaticorum_variable label "Étoile variable de type RS Canum Venaticorum".
• RS_Canum_Venaticorum_variable label "Переменная типа RS Гончих Псов".
• RS_Canum_Venaticorum_variable label "りょうけん座RS型変光星".
• RS_Canum_Venaticorum_variable label "獵犬座RS型變星".
• RS_Canum_Venaticorum_variable sameAs RS-Canum-Venaticorum-Stern.
• RS_Canum_Venaticorum_variable sameAs Estrella_variable_RS_Canum_Venaticorum.
• RS_Canum_Venaticorum_variable sameAs Étoile_variable_de_type_RS_Canum_Venaticorum.
• RS_Canum_Venaticorum_variable sameAs Variabile_RS_Canum_Venaticorum.
• RS_Canum_Venaticorum_variable sameAs りょうけん座RS型変光星.
• RS_Canum_Venaticorum_variable sameAs Gwiazdy_typu_RS_Canum_Venaticorum.
• RS_Canum_Venaticorum_variable sameAs m.07zkf5.
• RS_Canum_Venaticorum_variable sameAs Q1392913.
• RS_Canum_Venaticorum_variable sameAs Q1392913.
• RS_Canum_Venaticorum_variable sameAs RS_Canum_Venaticorum_variable.
• RS_Canum_Venaticorum_variable wasDerivedFrom RS_Canum_Venaticorum_variable?oldid=565663907.
• RS_Canum_Venaticorum_variable isPrimaryTopicOf RS_Canum_Venaticorum_variable.