Astronomy:V1017 Sagittarii
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Short description: Star in the constellation Sagittarius
250px Visual band light curves for the 1973 and 1991 eruptions of V1017 Sagittarii, adapted from Salazar et al. (2017)[1] | |
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| 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 |
| B−V color index | 0.39 |
| 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[2] mas |
| Distance | 1269+84 −60[3] pc |
| Absolute magnitude (MV) | +1.6 |
| Orbit | |
| Primary | white dwarf |
| Companion | giant star |
| Semi-major axis (a) | 16.1 R☉ |
| Eccentricity (e) | 0 (assumed) |
| Inclination (i) | 80+10 −8° |
| Details[2] | |
| white dwarf | |
| Mass | 1.1+0.03 −0.1 M☉ |
| giant star | |
| Mass | 0.60-0.79 M☉ |
| Radius | 5.3 R☉ |
| Luminosity | 18.5[lower-alpha 1] L☉ |
| Temperature | 5200 K |
| Other designations | |
| 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]
Notes
- ↑ Derived from given radius and temperature of star.
References
- ↑ 1.0 1.1 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. doi:10.1093/mnras/stx1161.
- ↑ 2.0 2.1 2.2 2.3 2.4 2.5 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G. Gaia DR2 record for this source at VizieR.
- ↑ 3.0 3.1 Schaefer, Bradley E. (2018). "The distances to Novae as seen by Gaia". Monthly Notices of the Royal Astronomical Society 481 (3): 3033–3051. doi:10.1093/mnras/sty2388. Bibcode: 2018MNRAS.481.3033S.
- ↑ "V1017 Sagittarii". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=V1017+Sagittarii.
- ↑ Mclaughlin, Dean B. (February 1946). "Nova Sagittarii 1919". Publications of the Astronomical Society of the Pacific 58 (340): 46-52. doi:10.1086/125779. Bibcode: 1946PASP...58...46M. https://articles.adsabs.harvard.edu/pdf/1946PASP...58...46M. 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. doi:10.1088/0067-0049/187/2/275. Bibcode: 2010ApJS..187..275S.
- ↑ 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. doi:10.1093/mnras/stz3424.
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