HR 7135

HR 7135 is a binary star system. Despite its Flamsteed designation of 62 Serpentis, the star can be found in the equatorial constellation of Aquila,[10] in front of a dark rift in the Milky Way near the constellation border.[5] It is visible to the naked eye as a dim, yellow-hued point of light with an apparent visual magnitude of 5.57.[2] The system is located 283 light years distant from the Sun, based on parallax,[1] and is drifting further away with a radial velocity of 23 km/s.[5]

Discovery of the binary nature of this system is credited to Canadian astronomer H. H. Plaskett in 1922. It is a single-lined spectroscopic binary with an orbital period of 8.2 years and an eccentricity of 0.24.[5][6] The visible component is an aging giant star with a stellar classification of G9 III,[3] having exhausted the supply of hydrogen at its core and expanded to 10.7[1] times the Sun's radius. It is a red clump giant, indicating it is on the horizontal branch and is generating energy via core helium fusion.[11] The star is 3.2[7] billion years old with 1.54[7] times the mass of the Sun. It is radiating 53[1] times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,666 K.[7] The star has a very low rate of spin, with the projected rotational velocity being too small to measure.[8]