Krüger 60
Krüger 60 is a binary star system located from Earth, being one of nearest stars. It is made up of a pair of red dwarf stars orbiting each other every 45 years.
Description
The larger, primary star is designated component A, while the secondary, smaller star is labeled component B. Component A has about 27% of the Sun's mass and 30% of the Sun's radius. Component B has about 18% of the Sun's mass and 21% of the Sun's radius.Image:DOCepLightCurve.png|250px|thumb|alt=|left|A blue band light curve for a flare on DO Cephei, adapted from Dal
In 1951, Peter van de Kamp and Sarah Lee Lippincott announced that component B is a flare star. It was given the variable star designation "DO Cephei". Flares lasting as long as one hour have been recorded.
This system is orbiting through the Milky Way at a distance from the core that varies from 7–9 kpc with an orbital eccentricity of 0.126–0.130. The closest approach to the Sun will occur in about 88,600 years when this system will come within.
Considering the orbit of the members of Krüger 60, detecting an exoplanet through radial velocity could prove difficult, as its orbit would be inclined only 13 degrees from our point of view, and create 1/5th as strong a radial velocity signal as an exoplanet orbiting edge-on from the point of view of the Solar System.