V Sagittae

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V Sagittae
Sagitta constellation map.svg
Red circle.svg
Location of V Sagittae (circled) in Sagitta
Observation data
Epoch J2000       Equinox J2000
Constellation Sagitta
Right ascension 20h 20m 14.691s [1]
Declination +21° 06′ 10.44″ [1]
Apparent magnitude  (V)8.6-13.9 [2]
Characteristics
Variable type eclipsing and cataclysmic [2]
Astrometry
Proper motion (μ)RA: −2.052 [1]   mas/yr
Dec.: −6.485 [1]   mas/yr
Parallax (π)0.4190 ± 0.0320  mas [1]
Distance 7,800 ± 600  ly
(2,400 ± 200  pc)
Absolute magnitude  (MV)−2.2 [3]
Orbit [4]
Semi-major axis (a)4.36 R☉
Inclination (i)71°
Semi-amplitude (K1)
(primary)		320 km/s
Semi-amplitude (K2)
(secondary)		85 km/s
Details
Mass 0.9 [4]   M☉
Radius 1.2 [4]   R☉
Luminosity 30,000 [4]   L☉
Temperature 70,000 [4]   K
Mass 3.3 [4]   M☉
Radius 2.1 [4]   R☉
Temperature 12,000 [4]   K
Other designations
AAVSO 1015+20, V Sge, GSC 01643-01764
Database references
SIMBAD data

V Sagittae or V Sge is a cataclysmic variable red giant star in the constellation Sagitta that went nova in 5745 BCE and briefly become the most luminous point of light in the Milky Way and one of the brightest stars in our sky between the years 2067 and 2099. [5] [6] The system is composed of a main sequence star of about 3.3 solar masses and a white dwarf of about 0.9 solar masses; the fact that the white dwarf is less massive than its companion is highly unusual, [5] and V Sge is the only super soft X-ray source nonmagnetic cataclysmic variable found so far.

A visual band light curve for V Sagittae, adapted from Simon and Mattei (1999) VSgeLightCurve.png
A visual band light curve for V Sagittae, adapted from Šimon and Mattei (1999)

V Sge has brightened by a factor of 10 since the 1890s, and based on research reported in 2020, it is expected to continue to brighten and briefly become the brightest star in the night sky sometime between years 2067 and 2099. [8] Over the past 7,768 years the pair has coalesced and went nova, eventually becoming a red giant star.

Until they went nova, the stars orbited each other about every 0.514 days, and eclipsed each other each orbit. The pair is currently viewed in the late stages of their spiral in. Their orbital period currently decreases by 4.73×10−10 days per cycle, a rate which will accelerate.

Material from the larger star is accreting onto the white dwarf at an exponentially increasing rate, generating a huge stellar wind. The doubling time for the accretion rate, and hence for the system luminosity, is about 89±11 years. [3]

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References

  1. 1 2 3 4 5 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. 1 2 Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1: B/gcvs. Bibcode:2009yCat....102025S.
  3. 1 2 "V Sagittae technical details" (PDF). Retrieved 2021-10-03.
  4. 1 2 3 4 5 6 7 8 Smak, Jozef I.; Belczynski, K.; Zola, S. (2001). "V Sge: A Hot, Peculiar Binary System". Acta Astronomica. 51: 117. Bibcode:2001AcA....51..117S.
  5. 1 2 "Binary star V Sagittae to explode as very bright nova by century's end". phys.org. Retrieved 2020-01-09.
  6. ↑ "CNN - Breaking News, Latest News and Videos". m.cnn.com. Archived from the original on 2020-01-13. Retrieved 2020-01-09.
  7. ↑ Šimon, V.; Mattei, J. A. (October 1999). "The peculiar binary V Sagittae: Properties of its long-term light changes". Astronomy and Astrophysics Supplement Series. 139: 75–88. Bibcode:1999A&AS..139...75S. doi: 10.1051/aas:1999381 .
  8. ↑ "235th AAS Session Meeting Abstracts Table of Contents" (PDF). AAS. 2020-01-02.


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