Avisual bandlight curve of V832 Cygni. The main plot shows the long-term variability, and the inset plot shows the variation over a single orbital period. Adapted from Harmanecet al. (2002)[8]
The primary component and brightest member of this system, designated 59 Cyg Aa, is a rapidly rotatingBe star with astellar classification of B1.5 Vnne.[3] This is a well-studied star thanks to pronounced spectral variations that have been observed since 1916, and two short-termshell star phases that were observed in 1973 and 1974–5.[9] It is actually a confirmedspectroscopic binary system with a high temperaturesubdwarfO-type companion in a 28-dayorbital period. The latter is heating the nearest side of the circumstellar gaseous disk that surrounds the primary.[6]
Orbiting the primary pair is 59 Cyg Ab, a magnitude 7.64A-type main-sequence star of class A3V, located at anangular separation of0.200″. A fourth component is a magnitude 9.8 A-typegiant star of class A8III at a separation of20.2″ along aposition angle (PA) of 352°, as of 2008. The fifth companion is magnitude 11.7 at a separation of26.7″ and a PA of 141°.[4]Gaia Data Release 2 suggests that the companions at20.2″ and26.7″ are respectively382 pc and366 pc away and moving in approximately the same direction as the primary triple.[10][11]
^abLesh, Janet Rountree (December 1968), "The Kinematics of the Gould Belt: an Expanding Group?",Astrophysical Journal Supplement,17: 371,Bibcode:1968ApJS...17..371L,doi:10.1086/190179.
