Sigma Serpentis
Sigma Serpentis, Latinized from σ Serpentis, is a star in the equatorial constellation Serpens. It is faintly visible to the naked eye with an apparent visual magnitude of +4.82. Based upon an annual parallax shift of 35.54 mas as seen from Earth, it is located 92 light-years from the Sun. The star is moving closer to the Sun with a radial velocity of −49 km/s.
Barry assigned this star a stellar classification of F3 V, indicating an ordinary F-type main-sequence star. It is about one billion years old and is spinning with a projected rotational velocity of 77.7 km/s. The star has an estimated 1.5 times the mass of the Sun and is radiating 7.2 times the Sun's luminosity from its photosphere at an effective temperature of.
A candidate red dwarf companion star, of spectral type M2V, was identified in 2012 by Kevin Luhman and collaborators. It is from the primary, corresponding to a projected separation of. Gaia DR3 astrometry confirms a similar parallax and proper motion.