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V1059 Sagittarii (also called Nova Sagittarii 1898) was a nova, which lit up in 1898[4] in the constellation Sagittarius. The star reached apparent magnitude 4.5, making it easily visible to the naked eye. It was discovered on 8 March 1898, by Williamina Fleming on a photographic plate taken at the Harvard College Observatory.[5] The discovery plate was an objective prism plate, part of the Henry Draper Memorial Photographs,[6] and Ms Fleming identified it as a nova based on its spectral characteristics.[7]

Nova Sagittarii 1898
Location of V1059 Sagittarii (circled in red)
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Sagittarius
Right ascension 19h 01m 50.556s[1]
Declination −13° 09′ 41.86″[1]
Apparent magnitude (V) 4.9(photographic) — 18.1(blue)[2]
Other designations
Nova Sgr 1898, V1059 Sgr, HD 176654, 2MASS J19015056-1309420, Gaia DR2 4198482401904374016
Database references
SIMBADdata
The light curve of nova V1059 Sagittarii, plotted from photographic magnitude data tabulated by Walker & Shapley.[3] The points listed with identical times were averaged before plotting.
The light curve of nova V1059 Sagittarii, plotted from photographic magnitude data tabulated by Walker & Shapley.[3] The points listed with identical times were averaged before plotting.

The astronomical literature contains a variety of values for V1059 Sagittarii's peak brightness. Özdönmez et al. list the peak magnitude as 2.0 (visual),[8] while Downes et al. report a much fainter value of magnitude 4.9 (photographic).[2] Novae are usually classified as "fast" or "slow" based on the time it takes the star to drop from peak brightness by more than 3 magnitudes (T3), but for this nova the decline from maximum was poorly observed, and no T3 value has been reported. Nonetheless, it is classified as a fast nova. Vogt et al. monitored the quiescent nova 116 years after the nova event, and saw minor (0.5 to 0.8 magnitude) variations occurring at irregular intervals, similar to low amplitude dwarf nova outbursts.[9]

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 V1059 Sagittarii, pair's orbital period is 6.866±0.017 hours.[10]


References


  1. Brown, 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.
  2. Downes, Ronald; Webbink, Ronald F.; Shara, Michael M. (1997). "A Catalog and Atlas of Cataclysmic Variables-Second Edition". Publications of the Astronomical Society of the Pacific. 109: 345–440. Bibcode:1997PASP..109..345D. doi:10.1086/133900. Retrieved 21 December 2020.
  3. Walker, Arville D.; Shapley, Harlow (January 1933). "The photographic light curves of thirteen novae". Annals of the Astronomical Observatory of Harvard College. 84 (7): 189–206. Bibcode:1933AnHar..84..189W. Retrieved 23 January 2021.
  4. Moore, Patrick (2006). The amateur astronomer. Patrick Moore's Practical Astronomy Series. Vol. 2005 (Illustrated 12th ed.). Birkhäuser. p. 293. ISBN 978-1-85233-878-7.
  5. 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 21 December 2020.
  6. Barker, George F. (1887). "On the Henry Draper Memorial Photographs of Stellar Spectra". Proceedings of the American Philosophical Society. 24 (125): 166–172. JSTOR 983130. Retrieved 21 December 2020.
  7. Pickering, E.C.; Fleming, W.P. (March 1899). "A new star in Sagittarius". The Astrophysical Journal. 9: 182–184. Bibcode:1899ApJ.....9..182P. doi:10.1086/140575. Retrieved 21 December 2020.
  8. Özdönmez, Aykut; Ege, Ergün; Güve, Tolga; Ak, Tansel (May 2018). "A New Catalogue of Galactic Novae: Investigation of the MMRDrelation & 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. Retrieved 21 December 2020.
  9. Vogt, N.; Tappert, C.; Puebla, E.C.; {Fuentes-Morales, I.; Ederoclite, A.; Schmidtobreick, L. (August 2018). "Life after eruption - VII. A search for stunted outbursts in 13 post-novae". Monthly Notices of the Royal Astronomical Society. 478 (4): 5427–5435. Bibcode:2018MNRAS.478.5427V. doi:10.1093/mnras/sty1445. Retrieved 21 December 2020.
  10. Thorstensen, John R.; Peters, Christopher S.; Skinner, Julie N. (November 2010). "Optical Studies of 20 Longer-Period Cataclysmic Binaries". Publications of the Astronomical Society of the Pacific. 122 (897): 1285. arXiv:1009.1265. Bibcode:2010PASP..122.1285T. doi:10.1086/657021. S2CID 16334234. Retrieved 21 December 2020.



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