V838 Herculis
Location of V838 Hercules (circled in red)
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Hercules
Right ascension 18h 46m 31.471s[1]
Declination +12° 14′ 02.10″[1]
Apparent magnitude (V) 5.3 Max.
19.1 Min.[2]
Characteristics
Variable type Nova,[2] eclipsing binary[3]
Astrometry
Proper motion (μ) RA: −2.691±1.666[1] mas/yr
Dec.: −6.600±1.930[1] mas/yr
Parallax (π)0.4642 ± 0.7106 mas[1]
Distance2530+3434
−636[2] pc
Other designations
Nova Her 1991, AAVSO 1841+12, Gaia DR2 4504548029183559552, 2MASS J18463156+1214007[4]
Database references
SIMBADdata

V838 Herculis, also known as Nova Herculis 1991, was a nova which occurred in the constellation Hercules in 1991. It was discovered by George Alcock of Yaxley, Cambridgeshire, England at 4:35 UT on the morning of 25 March 1991. He found it with 10×50 binoculars, and on that morning its apparent visual magnitude was 5 (making it visible to the naked eye). Palomar Sky Survey plates showed that before the outburst, the star was at photographic magnitude 20.6 (blue light) and 18.25 (red light).[5]

The light curve of V838 Herculis plotted from data presented in Woodward et al.[6] and AAVSO data

V838 Herculis declined from its peak brightness very quickly, fading by 2 magnitudes in less than three days, making it one of the fastest classical novae ever recorded.[7]

All novae are binary stars, with a "donor" star orbiting a white 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 often eclipsing binaries, and V838 Herculis does show such eclipses. The eclipses were first detected a few weeks after the nova outburst, and they show the system's orbital period to be 7 hours, 8 minutes and 36 seconds as of 1991. The shape of the eclipse light curve suggests that the white dwarf itself is not being eclipsed by the donor, but rather that the accretion disk surrounding the white dwarf is being partially eclipsed. The depth of the eclipses was initially only 0.1 magnitudes, but grew over the year following the nova event to 0.7 magnitudes, indicating that the accretion disk re-established itself after the nova outburst during that time.[3][7]

The white dwarf in the V838 Herculis system is an oxygen-neon-magnesium white dwarf,[8] with a mass of about 1.35 M☉, which is near the Chandrasekhar limit for white dwarf masses.[9][10] The donor star is believed to be a main sequence star.[11]

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 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.
  3. 1 2 Leibowitz, Elia M.; Mendelson, Haim; Mashal, Ezra; Prialnik, Dina; Seitter, Waltraut C. (February 1992). "The Presence of an Accretion Disk in the Eclipsing Binary System Nova Herculis 1991 Three Weeks after Outburst". Astrophysical Journal Letters. 385: L49. Bibcode:1992ApJ...385L..49L. doi:10.1086/186275. Retrieved 3 January 2021.
  4. ↑ "V838 Herculis". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-08-19.
  5. ↑ "V838 Her (Nova Herculis 1991)". aavso.org. AAVSO. Retrieved 2 January 2021.
  6. ↑ Woodward, Charles E.; Gehrz, R.D.; Jones, Terry J.; Lawrence, G.F. (January 1992). "The Peculiar, Fast Nova Herculis 1991". Astrophysical Journal Letters. 384: L41. Bibcode:1992ApJ...384L..41W. doi:10.1086/186258.
  7. 1 2 Ingram, Doug; Garnavich, Peter; Green, Paul; Szkody, Paula (June 1992). "Photometry and Spectroscopy of Nova Herculis 1991". Publications of the Astronomical Society of the Pacific. 104: 402. Bibcode:1992PASP..104..402I. doi:10.1086/133012. S2CID 122041406. Retrieved 3 January 2021.
  8. ↑ Matheson, Thomas; Filippenko, Alexei V.; Ho, Luis C. (November 1993). "Nova Herculis 1991: Thermonuclear Runaway on a Massive ONeMg White Dwarf". Astrophysical Journal Letters. 418: L29. Bibcode:1993ApJ...418L..29M. doi:10.1086/187108.
  9. ↑ Starrfield, S.; Iliadis, C.; Hix, W.R. (May 2016). "The Thermonuclear Runaway and the Classical Nova Outburst". Publications of the Astronomical Society of the Pacific. 128 (963): 051001. arXiv:1605.04294. Bibcode:2016PASP..128e1001S. doi:10.1088/1538-3873/128/963/051001. S2CID 118581319. Retrieved 3 January 2021.
  10. ↑ Hachisu, Izumi; Kato, Mariko (July 2018). "A Light Curve Analysis of Recurrent and Very Fast Novae in Our Galaxy, Magellanic Clouds, and M31". The Astrophysical Journal Supplement Series. 237 (1): 4. arXiv:1805.09932. Bibcode:2018ApJS..237....4H. doi:10.3847/1538-4365/aac833. S2CID 119184283.
  11. ↑ Hachisu, Izumi; Kato, Mariko (June 2019). "A Light-curve Analysis of 32 Recent Galactic Novae: Distances and White Dwarf Masses". The Astrophysical Journal Supplement Series. 242 (2): 18. arXiv:1905.10655. Bibcode:2019ApJS..242...18H. doi:10.3847/1538-4365/ab1b43. S2CID 166228785.
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