Epoch J2000.0 Equinox J2000.0
|Right ascension||21h 42m 42.804s|
|Declination||43° 35' 09.88"|
|Apparent magnitude (V)||7.7 — 12.4|
|Distance||372 ± 7 ly
(114 ± 2  pc)
SS Cygni is a variable star in the northern constellation Cygnus (the Swan). It is perhaps the prototype dwarf nova, meaning that it undergoes frequent and regular brightness outbursts - every 7 or 8 weeks in the case of this much-observed example. SS Cygni is often classified as a U Geminorum type dwarf nova. However, the maxima of SS Cygni are typically brighter than those of U Gem, rising from 12th magnitude to 8th magnitude for, typically, 1–2 days. The northerly declination of SS Cygni (about 44° N) makes the star almost circumpolar from European and North American latitudes, allowing a large proportion of the world's amateur astronomers to monitor its behaviour. Furthermore, since the star lies against the rich backdrop of the Milky Way band, the telescope field of view around SS Cygni contains an abundance of useful brightness comparison stars.
SS Cyg, like all other cataclysmic variables, consists of a close binary system. One of the components is a red dwarf-type star, cooler than our Sun, while the other is a white dwarf. Studies suggest that the stars in the SS Cyg system are separated (from surface to surface) by "only" 100,000 miles or less. In fact, the stars are so close that they complete their orbital revolution in slightly over 6 1/2 hours. The inclination of the system has been calculated to be about 50 degrees, yielding a respective component mass of 0.6 solar mass for the white dwarf primary star and 0.4 solar mass for the red dwarf secondary star.
Astronomically speaking, SS Cyg is also fairly close by. Originally thought to be at a distance of 90 to 100 light years from its Earth-bound admirers, its distance was revised in 1952 to about 400 light years. In 2007 Hubble Space Telescope data indicated a distance of about 540 light years, though this value caused difficulties with the theory of dwarf novae; this was checked during 2010—2012 using radio astrometry with VLBI, which yielded a smaller number (114 ± 2 parsecs or 372 ± 7 light-years). This value is much more in accord with the old (≈400 light-year) value, and it removes completely the difficulties the larger HST distance made for the theory of dwarf novae.
- Staff (2003). "V* SS Cyg -- Dwarf Nova". Centre de Données astronomiques de Strasbourg. Retrieved 2011-11-25.
- American Association of Variable Star Observers. "AAVSO Light Curve Generator". Retrieved 5 June 2013.
- J. C. A. Miller-Jones; G. R. Sivakoff; C. Knigge; E. G. Körding; M. Templeton; E. O. Waagen (24 May 2013). "An Accurate Geometric Distance to the Compact Binary SS Cygni Vindicates Accretion Disc Theory". Science 340 (6135): 950–952. arXiv:1305.5846. Bibcode:2013Sci...340..950M. doi:10.1126/science.1237145.
- Honey, W.B., et al. (1989). "Quiescent and Outburst Photometry of the Dwarf Nova SS Cygni". Monthly Notices of the Royal Astronomical Society 236: 727–734. Bibcode:1989MNRAS.236..727H. doi:10.1093/mnras/236.4.727.
- Burnham, Robert Jr. (1978). Burnham's Celestial Handbook. New York: Dover.
- M. R. Schreiber; J.P. Lasota (2007). "The dwarf nova SS Cygni: what is wrong?". Astronomy & Astrophysics 473 (3): 897–901. arXiv:0706.3888. Bibcode:2007A&A...473..897S. doi:10.1051/0004-6361:20078146.