HR Lyrae or Nova Lyrae 1919 was a nova which occurred in the constellationLyra in 1919. Its discovery was announced by Johanna C. Mackie on 6 December 1919. She discovered it while examining photographic plates taken at the Harvard College Observatory. The bulletin announcing the discovery (H.C.O. bulletin 705) states "Between December 4 and 6 it rose rapidly from the sixteenth magnitude or fainter, to a maximum of about 6.5". It was the first nova ever reported in Lyra, and Mackie was awarded the AAVSO gold medal for her discovery.[5][6] Its peak magnitude of 6.5 implies that it might have been visible to the naked eye, under ideal conditions.
The light curve of HR Lyrae, plotted from data presented in Shears & Poyner (2007)[3]
HR Lyrae's outburst occurred in December 1919, when Lyra was only visible in the early evening for most northern observers. Visibility was even more limited in the first months of 1920, so its light curve near maximum brightness is poorly sampled. But it is very likely that it declined from peak brightness by 3 magnitudes in less than 100 days, making it a "fast" nova. By November 1921 the star had dimmed to 14th magnitude, which is close to its quiescent brightness. It continues to show brightness fluctuations of 1 magnitude or less above its quiescent magnitude with no clear periodicity,[3][7] as well as dimming (down to 17th magnitude) episodes.[8][9] Although only one nova event has been seen, there are suggestions based primarily on the light curve that HR Lyrae might be a recurrent nova.[10]
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 HR Lyrae the binary's orbital period is uncertain, but a value of 2.4 hours has been reported.[11] The white dwarf's mass has been estimated to be 0.78±0.15M☉[12]
Referencesedit
^ abcdeBrown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
^ abSchaefer, Bradley E. (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.
^ abcShears, J.; Poyner, G. (June 2007). "HR Lyrae (Nova Lyr 1919): from outburst to active quiescence". Journal of the British Astronomical Association. 117 (3): 136–141. arXiv:astro-ph/0701719. Bibcode:2007JBAA..117..136S. Retrieved 24 December 2020.
^Duerbeck, Hilmar W. (March 1987). "A Reference Catalogue and Atlas of Galactic Novae". Space Science Reviews. 45 (1–2): 1–14. Bibcode:1987SSRv...45....1D. doi:10.1007/BF00187826. S2CID 115854775. Retrieved 24 December 2020.
^Poyner, Gary. "Observing through the light". AAVSO CV Section. AAVSO. Retrieved 24 December 2020.
^Honeycutt, R.K.; Shears, J.; Kafka, S.; Robertson, J.W.; Henden, A.A. (May 2014). "The 1991-2012 Light Curve of the Old Nova HR LYRAE". The Astronomical Journal. 147 (5): 105. Bibcode:2014AJ....147..105H. doi:10.1088/0004-6256/147/5/105. S2CID 119770018. Retrieved 25 December 2020.
^Shears, J.; Poyner, G. (December 2010). "A deep fade of HR Lyrae". Journal of the British Astronomical Association. 120: 380. Bibcode:2010JBAA..120..380S. Retrieved 25 December 2020.
^Munari, U.; Siviero, A.; Ochner, P.; Dallaporta, S. (August 2016). "Spectroscopy and photometry of HR Lyr (Nova Lyr 1919) during one of its mysterious dimming episodes". The Astronomer's Telegram. 9418: 1. Bibcode:2016ATel.9418....1M. Retrieved 25 December 2020.
^Pagnotta, Ashley; Schaefer, Bradley E. (June 2014). "Identifying and Quantifying Recurrent Novae Masquerading as Classical Novae". The Astrophysical Journal. 788 (2): 164. arXiv:1405.0246. Bibcode:2014ApJ...788..164P. doi:10.1088/0004-637X/788/2/164.
^Leibowitz, E.M.; Mendelson, H.; Gefen, G.; Retter, A. (January 1995). "Classical Novae as Wet Objects". Baltic Astronomy. 4 (4): 453–466. Bibcode:1995BaltA...4..453L. doi:10.1515/astro-1995-0405. S2CID 53001433.
^Selvelli, Pierluigi; Gilmozzi, Roberto (February 2019). "A UV and optical study of 18 old novae with Gaia DR2 distances: mass accretion rates, physical parameters, and MMRD". Astronomy & Astrophysics. 622: A186. arXiv:1903.05868. Bibcode:2019A&A...622A.186S. doi:10.1051/0004-6361/201834238.
lyrae, nova, lyrae, 1919, nova, which, occurred, constellation, lyra, 1919, discovery, announced, johanna, mackie, december, 1919, discovered, while, examining, photographic, plates, taken, harvard, college, observatory, bulletin, announcing, discovery, bullet. HR Lyrae or Nova Lyrae 1919 was a nova which occurred in the constellation Lyra in 1919 Its discovery was announced by Johanna C Mackie on 6 December 1919 She discovered it while examining photographic plates taken at the Harvard College Observatory The bulletin announcing the discovery H C O bulletin 705 states Between December 4 and 6 it rose rapidly from the sixteenth magnitude or fainter to a maximum of about 6 5 It was the first nova ever reported in Lyra and Mackie was awarded the AAVSO gold medal for her discovery 5 6 Its peak magnitude of 6 5 implies that it might have been visible to the naked eye under ideal conditions HR LyraeLocation of HR Lyrae circled in red Observation dataEpoch J2000 0 Equinox J2000 0 Constellation Lyra Right ascension 18h 53m 25 0564s 1 Declination 29 13 37 6664 1 Apparent magnitude V 6 5 Max 15 5 Min 2 Characteristics Variable type Classical Nova 3 AstrometryProper motion m RA 1 926 0 056 1 mas yr Dec 7 621 0 056 1 mas yrParallax p 0 1825 0 0337 mas 1 Distance4797 1015 470 2 pc Other designationsNova Lyrae 1919 Gaia DR2 2040551920255615104 HD 175268 2MASS J18532505 2913377 4 Database referencesSIMBADdata The light curve of HR Lyrae plotted from data presented in Shears amp Poyner 2007 3 HR Lyrae s outburst occurred in December 1919 when Lyra was only visible in the early evening for most northern observers Visibility was even more limited in the first months of 1920 so its light curve near maximum brightness is poorly sampled But it is very likely that it declined from peak brightness by 3 magnitudes in less than 100 days making it a fast nova By November 1921 the star had dimmed to 14th magnitude which is close to its quiescent brightness It continues to show brightness fluctuations of 1 magnitude or less above its quiescent magnitude with no clear periodicity 3 7 as well as dimming down to 17th magnitude episodes 8 9 Although only one nova event has been seen there are suggestions based primarily on the light curve that HR Lyrae might be a recurrent nova 10 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 HR Lyrae the binary s orbital period is uncertain but a value of 2 4 hours has been reported 11 The white dwarf s mass has been estimated to be 0 78 0 15M 12 References edit a b c d e Brown A G A et al Gaia collaboration August 2018 Gaia Data Release 2 Summary of the contents and survey properties Astronomy amp Astrophysics 616 A1 arXiv 1804 09365 Bibcode 2018A amp A 616A 1G doi 10 1051 0004 6361 201833051 Gaia DR2 record for this source at VizieR a b Schaefer Bradley E 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 a b c Shears J Poyner G June 2007 HR Lyrae Nova Lyr 1919 from outburst to active quiescence Journal of the British Astronomical Association 117 3 136 141 arXiv astro ph 0701719 Bibcode 2007JBAA 117 136S Retrieved 24 December 2020 HR Lyrae SIMBAD Centre de donnees astronomiques de Strasbourg Retrieved 2019 08 25 Duerbeck Hilmar W March 1987 A Reference Catalogue and Atlas of Galactic Novae Space Science Reviews 45 1 2 1 14 Bibcode 1987SSRv 45 1D doi 10 1007 BF00187826 S2CID 115854775 Retrieved 24 December 2020 Poyner Gary Observing through the light AAVSO CV Section AAVSO Retrieved 24 December 2020 Honeycutt R K Shears J Kafka S Robertson J W Henden A A May 2014 The 1991 2012 Light Curve of the Old Nova HR LYRAE The Astronomical Journal 147 5 105 Bibcode 2014AJ 147 105H doi 10 1088 0004 6256 147 5 105 S2CID 119770018 Retrieved 25 December 2020 Shears J Poyner G December 2010 A deep fade of HR Lyrae Journal of the British Astronomical Association 120 380 Bibcode 2010JBAA 120 380S Retrieved 25 December 2020 Munari U Siviero A Ochner P Dallaporta S August 2016 Spectroscopy and photometry of HR Lyr Nova Lyr 1919 during one of its mysterious dimming episodes The Astronomer s Telegram 9418 1 Bibcode 2016ATel 9418 1M Retrieved 25 December 2020 Pagnotta Ashley Schaefer Bradley E June 2014 Identifying and Quantifying Recurrent Novae Masquerading as Classical Novae The Astrophysical Journal 788 2 164 arXiv 1405 0246 Bibcode 2014ApJ 788 164P doi 10 1088 0004 637X 788 2 164 Leibowitz E M Mendelson H Gefen G Retter A January 1995 Classical Novae as Wet Objects Baltic Astronomy 4 4 453 466 Bibcode 1995BaltA 4 453L doi 10 1515 astro 1995 0405 S2CID 53001433 Selvelli Pierluigi Gilmozzi Roberto February 2019 A UV and optical study of 18 old novae with Gaia DR2 distances mass accretion rates physical parameters and MMRD Astronomy amp Astrophysics 622 A186 arXiv 1903 05868 Bibcode 2019A amp A 622A 186S doi 10 1051 0004 6361 201834238 External links edithttp www britastro org vss obj 18 html http astro corlan net stars LYR HR LYR html https web archive org web 20050909054008 http www tsm toyama toyama jp curators aroom var nova 1910 htm nbsp This variable star related article is a stub You can help Wikipedia by expanding it vte Retrieved from https en wikipedia org w index php title HR Lyrae amp oldid 1160585638, wikipedia, wiki, book, books, library,
