113 Herculis
113 Herculis is a binary star system located about away in the constellation Hercules. With an apparent magnitude of 4.6, it is faintly visible to the naked eye.
This star was first discovered to be a spectroscopic binary in 1900 by W. W. Campbell and W. H. Wright. The two stars orbit with a period of 245.3 days.
Charecterstics
113 Herculis is a spectroscopic double-line binary with an orbital period of 245.33 days and an eccentricity of 0.10. The system is estimated to be 391 million years old. It contains an evolved primary star, designated 113 Herculis Aa, and generally classified as a G-type yellow giant. It is a red clump star, meaning that it generates its energy by the fusion of helium in its core. It is estimated to be 3.15 times more massive than the Sun and its radius is nearly 24 times larger than the Sun's radius. Its surface temperature is. The Secondary component, 113 Herculis Ab, is a white main-sequence star of type A0 to A8. It is 2.18 times more massive than the Sun and its radius is 2.1 times larger than the solar radius. Its surface temperature is 9,183 K.Double and multiple star catalogs list two visual companions of magnitude 11.1 near 113 Herculis. Designated B and C, they were located at 34.4 and respectively from 113 Herculis A in 2001. Eggleton & Tokovinin proposed that these two stars are physically bound to the system, but measurements of their annual parallaxes of components B and C by the Gaia satellite show that they are much more distant, at distances of about and about respectively.