This system consists of two components, designated Kappa Pegasi A and B, that are separated by an angular distance of 0.235 arcseconds. The binary nature of this pair was discovered bySherburne W. Burnham in 1880. They orbit around each other every 11.6 years with asemimajor axis of 0.4 arcseconds. The brighter member of the pair, Kappa Pegasi B, is actually aspectroscopic binary, with the components designated Kappa Pegasi Ba and Kappa Pegasi Bb. They orbit about each other every six days. There is a fourth component, Kappa Pegasi C, which may be anoptical companion.[3]
^abcdPerryman, M. A. C.; et al. (April 1997). "The HIPPARCOS Catalogue".Astronomy & Astrophysics.323:L49 –L52.Bibcode:1997A&A...323L..49P.
^abJohnson, H. L.; Iriarte, B.; Mitchell, R. I.; Wisniewskj, W. Z. (1966). "UBVRIJKL photometry of the bright stars".Communications of the Lunar and Planetary Laboratory.4 (99): 99.Bibcode:1966CoLPL...4...99J.
^abBalachandran, Suchitra (May 1, 1990). "Lithium depletion and rotation in main-sequence stars".Astrophysical Journal, Part 1.354:310–332.Bibcode:1990ApJ...354..310B.doi:10.1086/168691.
^Bernacca, P. L.; Perinotto, M. (1970). "A catalogue of stellar rotational velocities".Contributi Osservatorio Astronomico di Padova in Asiago.239 (1): 1.Bibcode:1970CoAsi.239....1B.
