111 Herculis

111 Herculis is a suspected astrometric binary star system located 92 light years from the Sun in the northern constellation Hercules. It is visible to the naked eye as a faint, white-hued point of light with an apparent visual magnitude of 4.34. The system is moving nearer to the Earth with a heliocentric radial velocity of −45 km/s, and may come as close as 11.26 pc in 537,000 years.

According to Cowley et al. (1969), the visible component has a stellar classification of A5III, matching an A-type giant star. Abt and Morrell (1995) listed it as type A3IV, suggesting it is instead a less evolved subgiant star. The interferometry-measured angular diameter of the primary component is $0.148$, which, at its estimated distance, equates to a physical radius of roughly 1.6 times the radius of the Sun. The star is estimated to be 559 million years old with 2.40 times the mass of the Sun and is spinning with a projected rotational velocity of 71 km/s. It is radiating 13 times the Sun's luminosity from its photosphere at an effective temperature of 8,873 K.