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OY Arae

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OY Arae

Alight curvefor OY Arae. The main plot (from data published by Walker and Shapley)[1]shows the 1910 eruption, and the inset plot (adapted from Zhao and McClintock)[2]shows the eclipse light curve measured in 1995.
Observation data
EpochJ2000EquinoxJ2000
Constellation Ara
Right ascension 16h40m50.456s[3]
Declination −52° 25′ 47.98″[3]
Apparent magnitude(V) 18.7[4]
Characteristics
Apparent magnitude(B) 6.0 – 18.6[5]
B−Vcolor index −0.15[6]
Variable type Nova+eclipsing[5]
Astrometry
Proper motion(μ)RA:−3.689[3]mas/yr
Dec.:−3.182[3]mas/yr
Parallax(π)0.2676 ± 0.0714mas[3]
Distanceapprox. 12,000ly
(approx. 3,700pc)
Absolute magnitude(MV)−6.7 (at peak) 4.6 (quiescent)[7]
Orbit
Period(P)3.72936h[8]
Semi-major axis(a)1.28±0.04R☉[2]
Inclination(i)74.3±1.2[2]°
Details
white dwarf
Mass0.82±0.12[2]M☉
donor
Mass0.34±0.01[2]M☉
Other designations
Nova Arae 1910,HD149990,2MASSJ16405045-5225479
Database references
SIMBADdata

OY Arae,also known asNova Arae 1910,is anovain the constellationAra.It was discovered byWilliamina Flemingon aHarvard Observatoryphotographic platetaken on April 4, 1910. At that time it had a magnitude of 6.0, making it faintly visible to the naked eye under ideal observing conditions. Examination of earlier plates showed that before the outburst it was a magnitude 17.5 object, and by March 19, 1910, it had reached magnitude 12.[9][2]

OY Arae is considered to be a moderately fast nova, because it faded by 3 magnitudes during the 83 days after discovery.[10][9]The light curve shows a secondary maximum in June 1910. The first spectrum of the nova was obtained on July 5, 1910, and resembled that of a gaseous nebula.[11]An optical identification of the quiescent nova was made in 1994, and spectra taken at that time showed strongBalmer linesinemissionatop a blue continuum.[2]

All novae are binary stars, with a "donor" star orbiting awhite dwarf.The two stars are so close to each other that material is transferred from the donor to the white dwarf. Because the distance between the two stars is comparable to the radius of the donor star, novae are ofteneclipsing binaries,and OY Arae does show eclipses. The primary eclipse, in which the donor star eclipses the white dwarf and its accretion disk, are about 2 magnitudes deep and last less than 30 minutes. The orbital period is 3.73118 hours. The mass of the white dwarf is0.82±0.12M☉,and the mass of the donor star is 0.34±0.01M☉.The two stars are separated by1.28±0.04R☉.[2]

Most of theluminosityof the system is produced by the disk of material being stripped from the donor star. This is estimated to be 7 magnitudes brighter than the donor star itself, with the white dwarf being even fainter. Theabsolute magnitudeof the system is given as +4.6, but this value is distorted by the shape of the disk, seen nearly edge-on. A mean absolute magnitude adjusted for viewing angle is +3.6.[2]

References

[edit]
  1. ^Walker, Arville D.; Shapley, Harlow (January 1933). "The photographic light curves of thirteen novae".Annals of Harvard College Observatory.84(7): 189–206.Bibcode:1933AnHar..84..189W.
  2. ^abcdefghiZhao, Ping; McClintock, Jeffrey E. (July 1997)."A Dynamical Study of the Eclipsing Nova OY Arae".The Astrophysical Journal.483(2): 899–906.Bibcode:1997ApJ...483..899Z.doi:10.1086/304283.S2CID119710755.
  3. ^abcdeVallenari, A.; et al. (Gaia collaboration) (2023)."GaiaData Release 3. Summary of the content and survey properties ".Astronomy and Astrophysics.674:A1.arXiv:2208.00211.Bibcode:2023A&A...674A...1G.doi:10.1051/0004-6361/202243940.S2CID244398875. Gaia DR3 record for this sourceatVizieR.
  4. ^Howell, Steve B.; Mason, Elena (2018)."On the MV-Inclination Relationship for Nova-like Variables ".The Astronomical Journal.156(5): 198.arXiv:1808.08170.Bibcode:2018AJ....156..198H.doi:10.3847/1538-3881/aadd13.S2CID54503839.
  5. ^ab"OY Ara".The International Variable Star Index.AAVSO.Retrieved6 October2022.
  6. ^Duerbeck, H. W.; Seitter, W. C. (March 1987). "A Survey of Nova Remnants".Astrophysics and Space Science.131(1–2): 467–473.Bibcode:1987Ap&SS.131..467D.doi:10.1007/BF00668127.
  7. ^Warner, Brian (July 1987)."Absolute magnitudes of cataclysmic variables".Monthly Notices of the Royal Astronomical Society.227:23–73.Bibcode:1987MNRAS.227...23W.doi:10.1093/mnras/227.1.23.
  8. ^Sparks, Warren M.; Sion, Edward M. (2021)."Nova-produced Common Envelope: Source of the Nonsolar Abundances and an Additional Frictional Angular Momentum Loss in Cataclysmic Variables".The Astrophysical Journal.914(1): 16.arXiv:2103.14149.Bibcode:2021ApJ...914....5S.doi:10.3847/1538-4357/abf2bc.S2CID232380319.
  9. ^abDuerbeck, 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.S2CID115854775.
  10. ^Duerbeck, H. W. (April 1981)."Light curve types, absolute magnitudes, and physical properties of galactic novae".Publications of the Astronomical Society of the Pacific.93:165–175.Bibcode:1981PASP...93..165D.doi:10.1086/130799.S2CID121397724.
  11. ^Cannon, Annie Jump; Pickering, Edward Charles (1916). "Spectra having bright lines".Annals of the Astronomical Observatory of Harvard College.76(3): 19–42.Bibcode:1916AnHar..76...19C.
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