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  • 21 Aug, 2019

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V1494 Aquilae
V1494 Aquilae or Nova Aquilae 1999 b was a nova which occurred during 1999 in the constellation Aquila and reached a brightness of magnitude 3.9 on 2 December 1999. making it easily visible to the naked eye. The nova was discovered with 14×100 binoculars by Alfredo Pereira of Cabo da Roca, Portugal at 18:50 UT on 1 December 1999, when it had a visual magnitude of 6.0.

V1494 Aquilae is classified as a fast nova, meaning it faded from peak brightness by more than 3 magnitudes in less than 100 days. During its decline, V1494 Aql produced unusual variations in its x-ray radiation, including a bright burst lasting several minutes. During 2000, the x-ray spectrum developed from a hard (high energy) emission-line spectrum to a spectrum typical of a super soft X-ray source. The x-ray intensity varied with a period of about 40 minutes, probably due to pulsations induced in the white dwarf by its re-kindled hydrogen fusion.

All novae are binary systems with two stars orbiting so close to each other that one star, the "donor" star transfers matter to the other star which is a white dwarf. In the case of V1494 the white dwarf has a mass of 1.20M☉, and it is accreting mass from the donor star at a rate of 2.1 × 10 M☉ yr. The stars' orbital period is 3.23 hours, and the system is an eclipsing binary with two brightness minima each orbit, one 0.5 and one 0.1 magnitudes deep. This apparently is a measurement of two stars of approximately equal brightness, the nova and a companion 1.4″ to the south east. Measuring only the brightness of the nova, the eclipses are about two magnitudes deep. The white dwarf is probably an oxygen-neon-magnesium type.

Unlike some novae, the material ejected from V1494 Aquilae has not formed a visible nebula around the star. However, a shell approximately 6.5″ across has been detected spectroscopically in H-alpha emission.

The distance to V1494 Aquilae has been estimated by different methods. Early estimates were based on assumptions about the luminosity of the nova and gave distances around 1.2 kpc. Later models assumed distances of up to 2.2 kpc. Comparison of the measured shell size with the observed expansion velocity give a distance of 1.2±0.2 kpc. Gaia DR2 published a parallax of 0.8394±0.1415 mas, corresponding to a distance of 1,239+422
−127 kpc. Gaia EDR3 published a parallax of 0.5615±0.1281 mas, corresponding to a distance around 1,800 kpc.

References

  1. ^ "V1494 Aql". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-12-05.
  2. ^ Barsukova, E.A.; Goranskii, V.P. (March 2003). "The Orbital Period of Nova Aquilae 1999 No. 2 (V1494 Aql)". Astronomy Letters. 29 (3): 195–198. Bibcode:2003AstL...29..195B. doi:10.1134/1.1558159. S2CID 119929145.
  3. ^ 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.
  4. ^ Kato, Taichi; Ishioka, Ryoko; Uemura, Makoto; Starkey, Donn R.; Krajci, Tom (March 2004). "V1494 Aql: Eclipsing Fast Nova with an Unusual Orbital Light Curve". Publications of the Astronomical Society of Japan. 56: S125–S131. arXiv:astro-ph/0310519. Bibcode:2004PASJ...56S.125K. doi:10.1093/pasj/56.sp1.S125. S2CID 8328265.
  5. ^ Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  6. ^ Hachisu, Izumi; Kato, Mariko (2010). "A Prediction Formula of Supersoft X-Ray Phase of Classical Novae". The Astrophysical Journal. 709 (2): 680–714. arXiv:0912.1136. Bibcode:2010ApJ...709..680H. doi:10.1088/0004-637X/709/2/680. S2CID 118577218.
  7. ^ Hachisu, Izumi; Kato, Mariko; Kato, Taichi (2004). "Detection of Two-armed Spiral Shocks on the Accretion Disk of the Eclipsing Fast Nova V1494 Aquilae". The Astrophysical Journal. 606 (2): L139–L142. arXiv:astro-ph/0403589. Bibcode:2004ApJ...606L.139H. doi:10.1086/421295. S2CID 16575884.
  8. ^ Drake, Jeremy J.; Wagner, R. Mark; Starrfield, Sumner; Butt, Yousaf; Krautter, Joachim; Bond, H. E.; Della Valle, M.; Gehrz, R. D.; Woodward, Charles E.; Evans, A.; Orio, M.; Hauschildt, P.; Hernanz, M.; Mukai, K.; Truran, J. W. (2003). "The Extraordinary X-ray Light Curve of the Classical Nova V1494 Aquilae (1999 No. 2) in Outburst: The Discovery of Pulsations and a "Burst"". The Astrophysical Journal. 584 (1): 448–452. arXiv:astro-ph/0210072. Bibcode:2003ApJ...584..448D. doi:10.1086/345534. S2CID 14866037.
  9. ^ Nemiroff, R.; Bonnell, J., eds. (15 December 1999). "A Nova in Aquila". Astronomy Picture of the Day. NASA. Retrieved 7 December 2020.
  10. ^ Dicicco, D.; Vitorino, C.; Green, D.W.E. (December 1999). "Nova Aquilae 1999 No. 2". IAU Circular. 7323: 1. Bibcode:1999IAUC.7323....1D.
  11. ^ Ritter, H.; Kolb, U. (June 2003). "Catalogue of cataclysmic binaries, low-mass X-ray binaries and related objects (Seventh edition)". Astronomy & Astrophysics. 404: 301–303. arXiv:astro-ph/0301444. Bibcode:2003A&A...404..301R. doi:10.1051/0004-6361:20030330. S2CID 61117701.
  12. ^ Shara, Michael M.; Prialnik, Dina; Hillman, Yael; Kovetz, Attay (June 2018). "The Masses and Accretion Rates of White Dwarfs in Classical and Recurrent Novae". The Astrophysical Journal. 860 (2): 110. arXiv:1804.06880. Bibcode:2018ApJ...860..110S. doi:10.3847/1538-4357/aabfbd. S2CID 55851634.
  13. ^ Barsukova, E. A.; Valeev, A. F.; Goranskij, V. P.; Zharova, A. V. (October 2013). "Spectroscopic detection of resolved ejecta of nova V1494 Aql". The Astronomer's Telegram. 5454 (5454): 1. Bibcode:2013ATel.5454....1B.
  14. ^ Sahman, D.I.; Dhillon, V.S.; Knigge, C.; Marsh, T.R. (August 2015). "Searching for nova shells around cataclysmic variables". Monthly Notices of the Royal Astronomical Society. 451 (3): 2863–2876. arXiv:1505.06048. Bibcode:2015MNRAS.451.2863S. doi:10.1093/mnras/stv1150. S2CID 62784187.


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