V1974 Cygni or Nova Cygni 1992 was a nova, visible to the naked eye, in the constellationCygnus. It was discovered visually with 10×50 binoculars on February 19, 1992, by Peter Collins, an amateur astronomer living in Boulder, Colorado. At that time he first noticed it, it had an apparent magnitude of 7.2. Nine hours later he saw it again, and it had brightened by a full magnitude. For this discovery Collins was awarded the AAVSO Nova Award in 1993.[6][7] The nova reached magnitude 4.4 at 22:00 UT on 22 February 1992. Images from the Palomar Sky Survey taken before the nova event showed identified a possible precursor which had photographic magnitudes of 18 (blue light) and 17 (red light), but the identification of the precursor is not firm.[8][9]
V1974 Cygni
An HST image of V1974 Cygni, taken in January 1994, shortly after the repair mission to correct the HST's flawed optics.[1]
V1974 Cygni declined from peak brightness by three magnitudes in 43 days, making it a "fast" nova.[10] Its light curve is classified as type P (Plateau), and it may be a recurrent nova.[11]
In 1995, V1974 Cygni was observed with the Very Large Array at 1.49, 4.9, 8.4, 14.9 and 22.5 GHz.[12] It was also studied with the Hubble Space Telescope instrument the High Speed Photometer.[13] The instrument recorded a short amount of ultraviolet photometry.[13] The nova was also observed in the far-ultraviolet by Voyager 2.[14] It was observed, but not detected, with the Compton Gamma Ray Observatory.[15] It was the first nova to be observed throughout the electromagnetic spectrum, from radio waves to γ-rays.[16]
The location of V1974 Cygni (circled in red)
All novae are binary stars, with a "donor" star orbiting a white dwarf. The two stars are so close to each other that matter is transferred from the donor to the white dwarf. In the case of V1974 Cygni, the binary's orbital period is 1 hour, 57 minutes. The nova has an oxygen-neon-magnesium white dwarf primary, making it a neon nova.[9] Estimates of the mass of the white dwarf range from 0.98 M☉ to 1.12M☉, and it is estimated to be acquiring 3.2 × 10−10M☉ yr−1 of material from the donor star.[17]
V1974 Cygni has a nova remnant shell which has been observed several times with the Hubble Space Telescope, as well as with the Infrared Space Observatory. The shell is nearly circular, and its radius as of 10 February 1998 was 0.983 arc seconds. It is expanding at a rate of about 0.26 milli arc seconds per day.[16] The remnant was also imaged in 6 cm radio waves with the MERLIN interferometer.[12]
^"Nova Cygni 1992". esahubble.org. ESA. Retrieved 4 January 2021.
^ abCutri, Roc M.; Skrutskie, Michael F.; Van Dyk, Schuyler D.; Beichman, Charles A.; Carpenter, John M.; Chester, Thomas; Cambresy, Laurent; Evans, Tracey E.; Fowler, John W.; Gizis, John E.; Howard, Elizabeth V.; Huchra, John P.; Jarrett, Thomas H.; Kopan, Eugene L.; Kirkpatrick, J. Davy; Light, Robert M.; Marsh, Kenneth A.; McCallon, Howard L.; Schneider, Stephen E.; Stiening, Rae; Sykes, Matthew J.; Weinberg, Martin D.; Wheaton, William A.; Wheelock, Sherry L.; Zacarias, N. (2003). "VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)". CDS/ADC Collection of Electronic Catalogues. 2246: II/246. Bibcode:2003yCat.2246....0C.
^ abSchaefer, Bradley E. (December 2018). "The distances to Novae as seen by Gaia". Monthly Notices of the Royal Astronomical Society. 481 (3): 3033–3051. arXiv:1809.00180. Bibcode:2018MNRAS.481.3033S. doi:10.1093/mnras/sty2388. S2CID 118925493.
^Hurst, G.M. (June 1992). "Nova Cygni 1992". Journal of the British Astronomical Association. 102: 124. Bibcode:1992JBAA..102..124H.
^ abDe Young, James A.; Schmidt, Richard E. (August 1994). "The Photometric Period of V1974 Cygni (Nova Cygni 1992)". Astrophysical Journal Letters. 431: L47. Bibcode:1994ApJ...431L..47D. doi:10.1086/187469. Retrieved 4 January 2021.
^Özdönmez, Aykut; Ege, Ergün; Güver, Tolga; Ak, Tansel (May 2018). "A new catalogue of Galactic novae: investigation of the MMRD relation and spatial distribution". Monthly Notices of the Royal Astronomical Society. 476 (3): 4162–4186. arXiv:1802.05725. Bibcode:2018MNRAS.476.4162O. doi:10.1093/mnras/sty432. S2CID 73722195. Retrieved 4 January 2021.
^Strope, Richard J.; Schaefer, Bradley E.; Henden, Arne A. (July 2010). "Catalog of 93 Nova Light Curves: Classification and Properties". The Astronomical Journal. 140 (1): 34–62. arXiv:1004.3698. Bibcode:2010AJ....140...34S. doi:10.1088/0004-6256/140/1/34. S2CID 118537823. Retrieved 4 January 2021.
^ abHjellming, R.M (1995). Cataclysmic Variables. Vol. 205. Dordrecht: Springer. p. 139. Bibcode:1995ASSL..205..139H. ISBN978-94-010-4148-5. Retrieved 4 January 2021.
^ abUltraviolet photometry of Nova Cygni 1992 obtained with the high speed photometer
^Ulivi, Paolo; Harland, David M (2007). Robotic Exploration of the Solar System Part I: The Golden Age 1957-1982. Springer. p. 449. ISBN9780387493268.
^Shrader, C.R.; Gehrels, N. (July 1995). "Recent Results from the Compton Gamma Ray Observatory". Publications of the Astronomical Society of the Pacific. 107: 606. Bibcode:1995PASP..107..606S. doi:10.1086/133600. Retrieved 4 January 2021.
^ abKrautter, Joachim; Woodward, Charles E.; Schuster, Michael T.; Gehrz, Robert D.; Jones, Terry J.; Belle, Kunegunda; Evans, A.; Leyers, S.P.S.; Starrfield, Sumner; Truran, James; Greenhouse, Matthew A. (November 2002). "Hubble Space Telescope NICMOS Observations of Classical Nova Shells". The Astronomical Journal. 124 (5): 2888–2898. Bibcode:2002AJ....124.2888K. doi:10.1086/343833. Retrieved 4 January 2021.
^Shara, Michael M.; Prialnik, Dina; Hillman, Yael; Kovetz, Attay (June 2018). "The Masses and Accretion Rates of White Dwarfs in Classical and Recurrent Novae" (PDF). The Astrophysical Journal. 860 (2): 110. arXiv:1804.06880. Bibcode:2018ApJ...860..110S. doi:10.3847/1538-4357/aabfbd. S2CID 55851634. Retrieved 4 January 2021.
v1974, cygni, nova, cygni, 1992, nova, visible, naked, constellation, cygnus, discovered, visually, with, binoculars, february, 1992, peter, collins, amateur, astronomer, living, boulder, colorado, that, time, first, noticed, apparent, magnitude, nine, hours, . V1974 Cygni or Nova Cygni 1992 was a nova visible to the naked eye in the constellation Cygnus It was discovered visually with 10 50 binoculars on February 19 1992 by Peter Collins an amateur astronomer living in Boulder Colorado At that time he first noticed it it had an apparent magnitude of 7 2 Nine hours later he saw it again and it had brightened by a full magnitude For this discovery Collins was awarded the AAVSO Nova Award in 1993 6 7 The nova reached magnitude 4 4 at 22 00 UT on 22 February 1992 Images from the Palomar Sky Survey taken before the nova event showed identified a possible precursor which had photographic magnitudes of 18 blue light and 17 red light but the identification of the precursor is not firm 8 9 V1974 CygniAn HST image of V1974 Cygni taken in January 1994 shortly after the repair mission to correct the HST s flawed optics 1 Observation dataEpoch J2000 0 Equinox J2000 0Constellation CygnusRight ascension 20h 30m 31 61s 2 Declination 52 37 51 3 2 Apparent magnitude V 4 3 max gt 21 min 3 AstrometryDistance1631 261 131 3 pcCharacteristicsVariable type neon nova 4 Other designationsNova Cyg 1975 AAVSO 2027 52 V1974 Cyg 2MASS J20303161 5237513 5 Database referencesSIMBADdataThe light curve of V1974 Cygni plotted from AAVSO data V1974 Cygni declined from peak brightness by three magnitudes in 43 days making it a fast nova 10 Its light curve is classified as type P Plateau and it may be a recurrent nova 11 In 1995 V1974 Cygni was observed with the Very Large Array at 1 49 4 9 8 4 14 9 and 22 5 GHz 12 It was also studied with the Hubble Space Telescope instrument the High Speed Photometer 13 The instrument recorded a short amount of ultraviolet photometry 13 The nova was also observed in the far ultraviolet by Voyager 2 14 It was observed but not detected with the Compton Gamma Ray Observatory 15 It was the first nova to be observed throughout the electromagnetic spectrum from radio waves to g rays 16 The location of V1974 Cygni circled in red All novae are binary stars with a donor star orbiting a white dwarf The two stars are so close to each other that matter is transferred from the donor to the white dwarf In the case of V1974 Cygni the binary s orbital period is 1 hour 57 minutes The nova has an oxygen neon magnesium white dwarf primary making it a neon nova 9 Estimates of the mass of the white dwarf range from 0 98 M to 1 12M and it is estimated to be acquiring 3 2 10 10 M yr 1 of material from the donor star 17 V1974 Cygni has a nova remnant shell which has been observed several times with the Hubble Space Telescope as well as with the Infrared Space Observatory The shell is nearly circular and its radius as of 10 February 1998 was 0 983 arc seconds It is expanding at a rate of about 0 26 milli arc seconds per day 16 The remnant was also imaged in 6 cm radio waves with the MERLIN interferometer 12 See also EditNova Cygni 1975References Edit Nova Cygni 1992 esahubble org ESA Retrieved 4 January 2021 a b Cutri Roc M Skrutskie Michael F Van Dyk Schuyler D Beichman Charles A Carpenter John M Chester Thomas Cambresy Laurent Evans Tracey E Fowler John W Gizis John E Howard Elizabeth V Huchra John P Jarrett Thomas H Kopan Eugene L Kirkpatrick J Davy Light Robert M Marsh Kenneth A McCallon Howard L Schneider Stephen E Stiening Rae Sykes Matthew J Weinberg Martin D Wheaton William A Wheelock Sherry L Zacarias N 2003 VizieR Online Data Catalog 2MASS All Sky Catalog of Point Sources Cutri 2003 CDS ADC Collection of Electronic Catalogues 2246 II 246 Bibcode 2003yCat 2246 0C a b Schaefer Bradley E December 2018 The distances to Novae as seen by Gaia Monthly Notices of the Royal Astronomical Society 481 3 3033 3051 arXiv 1809 00180 Bibcode 2018MNRAS 481 3033S doi 10 1093 mnras sty2388 S2CID 118925493 Hachisu Izumi Kato Mariko January 2016 Light curve Analysis of Neon Novae The Astrophysical Journal 816 1 26 arXiv 1511 06819 Bibcode 2016ApJ 816 26H doi 10 3847 0004 637X 816 1 26 S2CID 118690985 V1974 Cygni SIMBAD Centre de donnees astronomiques de Strasbourg Retrieved 2021 01 04 Peter Collins Discovered V1974 Cygni With Binoculars Feb 19 1992 Earth and Space News Earth and Space News Retrieved 4 January 2021 V1974 Cyg Nova Cygni 1992 aavso org AAVSO Retrieved 4 January 2021 Hurst G M June 1992 Nova Cygni 1992 Journal of the British Astronomical Association 102 124 Bibcode 1992JBAA 102 124H a b De Young James A Schmidt Richard E August 1994 The Photometric Period of V1974 Cygni Nova Cygni 1992 Astrophysical Journal Letters 431 L47 Bibcode 1994ApJ 431L 47D doi 10 1086 187469 Retrieved 4 January 2021 Ozdonmez Aykut Ege Ergun Guver Tolga Ak Tansel May 2018 A new catalogue of Galactic novae investigation of the MMRD relation and spatial distribution Monthly Notices of the Royal Astronomical Society 476 3 4162 4186 arXiv 1802 05725 Bibcode 2018MNRAS 476 4162O doi 10 1093 mnras sty432 S2CID 73722195 Retrieved 4 January 2021 Strope Richard J Schaefer Bradley E Henden Arne A July 2010 Catalog of 93 Nova Light Curves Classification and Properties The Astronomical Journal 140 1 34 62 arXiv 1004 3698 Bibcode 2010AJ 140 34S doi 10 1088 0004 6256 140 1 34 S2CID 118537823 Retrieved 4 January 2021 a b Hjellming R M 1995 Cataclysmic Variables Vol 205 Dordrecht Springer p 139 Bibcode 1995ASSL 205 139H ISBN 978 94 010 4148 5 Retrieved 4 January 2021 a b Ultraviolet photometry of Nova Cygni 1992 obtained with the high speed photometer Ulivi Paolo Harland David M 2007 Robotic Exploration of the Solar System Part I The Golden Age 1957 1982 Springer p 449 ISBN 9780387493268 Shrader C R Gehrels N July 1995 Recent Results from the Compton Gamma Ray Observatory Publications of the Astronomical Society of the Pacific 107 606 Bibcode 1995PASP 107 606S doi 10 1086 133600 Retrieved 4 January 2021 a b Krautter Joachim Woodward Charles E Schuster Michael T Gehrz Robert D Jones Terry J Belle Kunegunda Evans A Leyers S P S Starrfield Sumner Truran James Greenhouse Matthew A November 2002 Hubble Space Telescope NICMOS Observations of Classical Nova Shells The Astronomical Journal 124 5 2888 2898 Bibcode 2002AJ 124 2888K doi 10 1086 343833 Retrieved 4 January 2021 Shara Michael M Prialnik Dina Hillman Yael Kovetz Attay June 2018 The Masses and Accretion Rates of White Dwarfs in Classical and Recurrent Novae PDF The Astrophysical Journal 860 2 110 arXiv 1804 06880 Bibcode 2018ApJ 860 110S doi 10 3847 1538 4357 aabfbd S2CID 55851634 Retrieved 4 January 2021 External links Edithttps web archive org web 20050915104557 http www tsm toyama toyama jp curators aroom var nova 1990 htm http www aavso org v1974 cyg nova cygni 1992 Retrieved from https en wikipedia org w index php title V1974 Cygni amp oldid 1136116923, wikipedia, wiki, book, books, library,
