Astronomy:SS Cygni
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Cygnus |
| Right ascension | 21h 42m 42.8034s[2] |
| Declination | +43° 35′ 09.864″[2] |
| Apparent magnitude (V) | 7.7–12.4[3] |
| Characteristics | |
| Spectral type | K5V[4] |
| Variable type | Dwarf nova[3] |
| Astrometry | |
| Radial velocity (Rv) | −6.3±2.3[5] km/s |
| Proper motion (μ) | RA: 112.373±0.113[2] mas/yr Dec.: 33.589±0.094[2] mas/yr |
| Parallax (π) | 8.7242 ± 0.0491[2] mas |
| Distance | 372±7 ly (114±2[6] pc) |
| Orbit[5] | |
| Period (P) | 0.27512973[7] days |
| Semi-major axis (a) | 1.51–1.77 R☉ |
| Inclination (i) | 45–56° |
| Semi-amplitude (K1) (primary) | 71.4±1.6 km/s |
| Semi-amplitude (K2) (secondary) | 158.6±0.7 km/s |
| Details[5] | |
| Red dwarf | |
| Mass | 0.19–0.30 M☉ |
| Temperature | 4,560[7] K |
| White dwarf | |
| Mass | 0.42–0.67 M☉ |
| Other designations | |
| Database references | |
| SIMBAD | data |
SS Cygni is a variable star in the northern constellation Cygnus (the Swan). It was discovered in 1896 by Louisa D. Wells, a computer working under Edward Pickering at Harvard College Observatory.[8][9] It is the prototype of the subclass of dwarf novae that show only normal eruptions. It typically rises from 12th magnitude to 8th magnitude for 1–2 days every 7 or 8 weeks. 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 behavior. 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 Cygni, like all other cataclysmic variables, consists of a close binary system. One of the components is a red dwarf-type star, cooler than the Sun, while the other is a white dwarf. The stars in the SS Cygni system are separated by a distance "only" 1.51 times larger than the Sun,[7] completing their orbital revolution in slightly over six hours and 36 minutes. The inclination of the system is estimated to be 45-56 degrees, yielding masses in the range of 0.42–0.67 M☉ for the white dwarf primary star and 0.19–0.30 M☉ for the red dwarf secondary star.[5]
Astronomically speaking, SS Cygni is also fairly close by. Originally thought to be at 90 to 100 light years,[10] 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;[11] this was checked during 2010–2012 using radio astrometry with VLBI, which yielded a smaller distance of 114 ± 2 parsecs (371.8 ± 6.5 ly).[6] 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.
References
- ↑ "Download Data". AAVSO. https://www.aavso.org/data-download.
- ↑ 2.0 2.1 2.2 2.3 2.4 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G. Gaia DR2 record for this source at VizieR.
- ↑ 3.0 3.1 Samus, N. N. et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007–2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S 1. Bibcode: 2009yCat....102025S.
- ↑ North, R. C; Marsh, T. R; Kolb, U; Dhillon, V. S; Moran, C. K. J (2002). "The systemic velocities of four long-period cataclysmic variable stars". Monthly Notices of the Royal Astronomical Society 337 (4): 1215–1223. doi:10.1046/j.1365-8711.2002.05795.x. Bibcode: 2002MNRAS.337.1215N.
- ↑ 5.0 5.1 5.2 5.3 Zamora, I Mora; Echevarría, J.; Sánchez, L. J.; Ramírez, S. H. (2025-04-25). "A new radial velocity study of the well-known dwarf nova SS Cygni: a low-mass binary system" (in en). Monthly Notices of the Royal Astronomical Society 539 (3): 2055–2063. doi:10.1093/mnras/staf612. ISSN 0035-8711.
- ↑ 6.0 6.1 J. C. A. Miller-Jones; G. R. Sivakoff; C. Knigge; E. G. Körding et al. (24 May 2013). "An Accurate Geometric Distance to the Compact Binary SS Cygni Vindicates Accretion Disc Theory". Science 340 (6135): 950–952. doi:10.1126/science.1237145. PMID 23704566. Bibcode: 2013Sci...340..950M.
- ↑ 7.0 7.1 7.2 Bitner, Martin A; Robinson, Edward L; Behr, Bradford B (2007). "The Masses and Evolutionary State of the Stars in the Dwarf Nova SS Cygni". The Astrophysical Journal 662 (1): 564–573. doi:10.1086/517496. Bibcode: 2007ApJ...662..564B.
- ↑ "Cygnus' famous stellar duo: 61 Cyg and SS Cyg – Astronomy Now" (in en-US). https://astronomynow.com/2023/07/31/cygnus-famous-stellar-duo-61-cyg-and-ss-cyg/.
- ↑ Ogilvie, Marilyn Bailey, and Joy Dorothy Harvey. The Biographical Dictionary of Women in Science: Pioneering Lives from Ancient Times to the Mid-20th Century. New York: Routledge, 2000, 1363.
- ↑ Burnham, Robert Jr. (1978). Burnham's Celestial Handbook. New York: Dover. https://archive.org/details/burnhamscelestia02robe.
- ↑ M. R. Schreiber; J.P. Lasota (2007). "The dwarf nova SS Cygni: what is wrong?". Astronomy & Astrophysics 473 (3): 897–901. doi:10.1051/0004-6361:20078146. Bibcode: 2007A&A...473..897S.
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