Astronomy:V1500 Cygni
 Nova Cygni 1975 (center), photographed at 07:00 UT August 30, 1975. Also shown are 59 Cygni (magnitude 4.8), 60 Cygni (magnitude 5.4) and 63 Cygni (magnitude 4.5) | |
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Cygnus |
| Right ascension | 21h 11m 36.5810s[1] |
| Declination | +48° 09′ 01.952″[1] |
| Apparent magnitude (V) | 1.69 to <21[2] |
| Characteristics | |
| Variable type | Fast nova[2] + asynchronous polar[3] |
| Astrometry | |
| Proper motion (μ) | RA: −6.449(131)[1] mas/yr Dec.: −5.572(112)[1] mas/yr |
| Parallax (π) | 0.6427 ± 0.1087[1] mas |
| Distance | approx. 5,100 ly (approx. 1,600 pc) |
| Absolute magnitude (MV) | −10.7 (maximum)[4] to +7.8 (minimum)[5] |
| Details | |
| WD | |
| Mass | 1.20[6] M☉ |
| Radius | 0.009[7] R☉ |
| Luminosity | 5[7] L☉ |
| Temperature | 54,000[5] K |
| donor | |
| Mass | ~0.22[8] M☉ |
| Radius | 0.42[5] R☉ |
| Temperature | 3,000 - 5,200[5] K |
| Other designations | |
Nova Cyg 1975, AAVSO 2108+47[9] | |
| Database references | |
| SIMBAD | data |
V1500 Cygni or Nova Cygni 1975 was a bright nova occurring in 1975 in the constellation Cygnus. It had the second highest intrinsic brightness of any nova of the 20th century, exceeded only by CP Puppis in 1942.[10]
V1500 Cygni was discovered shining at an apparent brightness of magnitude 3.0 by Minoru Honda of Kurashiki, Japan on 29 August 1975.[11] It had brightened to magnitude 1.7 on the next day, and then rapidly faded. It remained visible to the naked eye for about a week, and 680 days after reaching maximum the star had dimmed by 12.5 magnitudes.
It is an AM Herculis type star, consisting of a red dwarf secondary depositing a stream of material onto a highly magnetized white dwarf primary. The distance of the V1500 Cygni was calculated in 1977 by the McDonald Observatory at 1.95 kiloparsecs (6,360 light years).[12] More recently the Gaia space observatory determined a distance of approximately 5,100 light years.[1] Additionally, V1500 Cyg was the first asynchronous polar to be discovered. This distinction refers to the fact that the white dwarf's spin period is slightly different from the binary orbital period.[13]
See also
- Nova Cygni 1920
- Nova Cygni 1992
References
- ↑ 1.0 1.1 1.2 1.3 1.4 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940 Gaia DR3 record for this source at VizieR.
- ↑ 2.0 2.1 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: B/gcvs. Bibcode: 2009yCat....102025S.
- ↑ Pavlenko, E. P.; Mason, P. A.; Sosnovskij, A. A.; Shugarov, S. Yu; Babina, Ju V.; Antonyuk, K. A.; Andreev, M. V.; Pit, N. V. et al. (2018). "Asynchronous polar V1500 Cyg: Orbital, spin, and beat periods". Monthly Notices of the Royal Astronomical Society 479 (1): 341. doi:10.1093/mnras/sty1494. Bibcode: 2018MNRAS.479..341P.
- ↑ Harrison, Thomas E.; Campbell, Ryan K. (2016). "The apparent synchronization of V1500 Cygni". Monthly Notices of the Royal Astronomical Society 459 (4): 4161. doi:10.1093/mnras/stw961. Bibcode: 2016MNRAS.459.4161H.
- ↑ 5.0 5.1 5.2 5.3 Harrison, Thomas E.; Campbell, Ryan K. (2018). "The detection of discrete cyclotron emission features in phase-resolved optical spectroscopy of V1500 Cygni". Monthly Notices of the Royal Astronomical Society 474 (2): 1572. doi:10.1093/mnras/stx2881. Bibcode: 2018MNRAS.474.1572H.
- ↑ Hachisu, Izumi; Kato, Mariko (2019). "A Light-curve Analysis of 32 Recent Galactic Novae: Distances and White Dwarf Masses". The Astrophysical Journal Supplement Series 242 (2): 18. doi:10.3847/1538-4365/ab1b43. Bibcode: 2019ApJS..242...18H.
- ↑ 7.0 7.1 Schmidt, Gary D.; Liebert, James; Stockman, H. S. (1995). "Detection of the Hot White Dwarf in the Magnetic Nova V1500 Cygni with the Hubble Space Telescope". The Astrophysical Journal 441: 414. doi:10.1086/175365. Bibcode: 1995ApJ...441..414S.
- ↑ Wang, Qishan; Qian, Shengbang; Liao, Wenping (1 November 2021). "Photometric Analysis of the TESS Light Curve for the Asynchronous Polar V1500 Cyg". Publications of the Astronomical Society of the Pacific 133 (1029). doi:10.1088/1538-3873/ac27f9. Bibcode: 2021PASP..133k4201W.
- ↑ "V1500 Cyg". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=V1500+Cyg.
- ↑ "V1500 Cyg (Nova Cygni 1975)". http://www.aavso.org/v1500-cyg-nova-cygni-1975.
- ↑ "V1500 Cyg (Nova Cygni 1975)". AAVSO. https://www.aavso.org/v1500-cyg-nova-cygni-1975.
- ↑ Ferland, G. J. (1977). "The interstellar reddening and distance of Nova Cygni 1975 /V1500 Cygni/". Astrophysical Journal 215: 873. doi:10.1086/155424. Bibcode: 1977ApJ...215..873F.
- ↑ Stockman, H. S.; Schmidt, Gary D.; Lamb, D. Q. (1988). "V1500 Cygni - Discovery of a magnetic nova". The Astrophysical Journal 332: 282. doi:10.1086/166652. Bibcode: 1988ApJ...332..282S.
Further reading
- Ferland GJ; Tomkin J; Woodman J (1976). "Continuum variability in Nova Cygni 1975". Nature 264 (5587): 627–9. doi:10.1038/264627a0. Bibcode: 1976Natur.264..627F.
External links
- "Detail for V1500 Cygni". The International Variable Star Index. http://www.aavso.org/vsx/index.php?view=detail.top&oid=12420.
- "Nova Cygni 1975 (V1500 Cygni)". The Encyclopedia of Astrobiology, Astronomy and Spaceflight. http://www.daviddarling.info/encyclopedia/N/Nova_Cygni_1975.html. Retrieved 2005-08-12.
- "V1500 Cyg (Nova Cygni 1975)". American Association of Variable Star Observers. http://www.aavso.org/v1500-cyg-nova-cygni-1975.
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