V1017 Sagittarii
 Visual band light curves for the 1973 and 1991 eruptions of V1017 Sagittarii, adapted from Salazar et al. (2017)[1] | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Sagittarius |
| Right ascension | 18h 32m 04.4738s[2] |
| Declination | −29° 23′ 12.5935″[2] |
| Apparent magnitude (V) | 4.5±2 Max. 13.5 Min.[3] |
| Characteristics | |
| Spectral type | G5IIIp / white dwarf |
| Variable type | eclipsing recurrent nova (NR+E) |
| Astrometry | |
| Radial velocity (Rv) | 15 km/s |
| Proper motion (μ) | RA: 5.241±0.086[2] mas/yr Dec.: −10.392±0.066[2] mas/yr |
| Parallax (π) | 0.7892±0.0437 mas[2] |
| Distance | 1269+84 −60[3] pc |
| Other designations | |
| Nova Sagittarii 1919, AAVSO 1825-29, Gaia DR2 4048251562703375488, 2MASS J18320447-2923125[4] | |
| Database references | |
| SIMBAD | data |
V1017 Sagittarii is a cataclysmic variable star system in the constellation Sagittarius. Ida E. Woods discovered the star on Harvard College Observatory photographic plates, in 1919.[5] During that eruption, the star reached magnitude 7. Its other eruptions in 1901, 1973 and 1991 only reached magnitude 10, leading it to be reclassified from a recurrent nova to a dwarf nova.[6]
After the eruption of 1919, the orbital period of the binary system has decreased by 0.0273±0.0061%, to the 5.786290±0.000032 days.[1] Physical models cannot explain the orbital change of such sign and magnitude as in 2019.[7]
References
[edit]- ^ a b Salazar, Irene V.; Lebleu, Amy; Schaefer, Bradley E.; Landolt, Arlo U.; Dvorak, Shawn (2017). "Accurate pre- and post-eruption orbital periods for the dwarf/Classical nova V1017 SGR". Monthly Notices of the Royal Astronomical Society. 469 (4): 4116–4132. arXiv:1612.00405. doi:10.1093/mnras/stx1161.
- ^ 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 & 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.
- ^ 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.
- ^ "V1017 Sagittarii". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-08-25.
- ^ Mclaughlin, Dean B. (February 1946). "Nova Sagittarii 1919". Publications of the Astronomical Society of the Pacific. 58 (340): 46–52. Bibcode:1946PASP...58...46M. doi:10.1086/125779. Retrieved 5 October 2025.
- ^ Schaefer, Bradley E. (2010). "Comprehensive Photometric Histories of All Known Galactic Recurrent Novae". The Astrophysical Journal Supplement. 187 (2): 275–373. arXiv:0912.4426. Bibcode:2010ApJS..187..275S. doi:10.1088/0067-0049/187/2/275. S2CID 119294221.
- ^ Schaefer, Bradley E. (2020). "Sudden and steady orbital period changes across six classical Nova Eruptions: The end of hibernation and two serious challenges for the magnetic braking model of cataclysmic variable evolution". Monthly Notices of the Royal Astronomical Society. 492 (3): 3343–3358. arXiv:1912.06170. doi:10.1093/mnras/stz3424.
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