RS Canum Venaticorum variable

Otto 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:

• Regular systems. Orbital periods are 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 eclipse.
• Short period systems. Components are detached and orbital periods are 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.
• Long period systems. Orbital periods is 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 eclipse.

• Flare star systems. In this case the hotter component is of the spectral type dKe or dMe, where the emission refers to strong Ca II H and K.
• 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 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 type stars 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 L_x >> 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