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V533 Herculis

V533 Herculis

RGB composite color image of the faint shell surrounding V533 Herculis, made from three narrow band images: Blue = 4800Å, green = Hα at 6563 Å and red = [NII] at 6583 Å. From Santamaria et al. 2020[1]
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Hecules
Right ascension 18h 14m 20.485s[2]
Declination +41° 51′ 22.07″[2]
Apparent magnitude (V) 3.0 - 15.0[3]
Astrometry
Distance1202+52
−41[3] pc
Characteristics
Variable type Classical Nova
Other designations
V533 Her, Nova Her 1963, AAVSO 1811+41
Database references
SIMBADdata
Visual band light curve of V533 Herculis, plotted using AAVSO data

V533 Herculis was a nova visible to the naked eye, which occurred in 1963 in the constellation of Hercules.[4]

The nova was discovered by the Swedish amateur astronomer Elis Dahlgren on 6 February 1963, and independently by an American amateur, Leslie Peltier, on 7 February 1963.[5][6] Both reported it to be a 4th magnitude star.[7] Subsequent examination of pre-discovery images, taken by the Baker-Nunn satellite tracking group at the Tokyo Observatory, showed that the star had begun its nova event as early as 18:36 UT on 26 January 1963, when it had an magnitude of 8. It had attained its peak brightness, magnitude 3, by 17:38 UT on 30 January 1968.[6]

All novae are binary stars, with a "donor" star transferring matter to a white dwarf. In the case of V533 Herculis, the pair's orbital period is 3.43 hours.[8] Thorstensen and Taylor analysed spectra of the star in its quiescent state, and concluded that it is a non-eclipsing SW Sextantis variable, implying that the donor star is a red dwarf.[9] Knigge derived a mass of 0.225 M⊙, and a radius of 0.333 R⊙, for the donor star.[10]

Two images of the shell surrounding V533 Hercules taken 25 years apart, showing the nebula's expansion. Both were taken with Hα filters, left at the William Herschel Telescope, and right with the Nordic Optical Telescope.[1]

Images of V533 Herculis taken with the Hubble Space Telescope show a faint, approximately circular shell (nebula) with a diameter of 10±1.4 arc seconds, surrounding the star. The shell is expanding at 850±150 km/sec.[11] Santamaria et al. obtained similar results by comparing images of the shell taken in 1993 and 2018. They found that by 2018 the slightly elliptical shell had major and minor axis of 16.8×15.2 arc seconds, and it was expanding at a rate of 0.152×0.139 arc seconds per year, implying a physical expansion rate of 850×770 km/sec.[1]

The location of V533 Herculis (circled in red)

References

  1. ^ a b c Santamaria, E.; Guerrero, M.A.; Ramos-Larios, G.; Toala, J.A.; Sabin, L.; Rubio, G.; Quino-Mendoza, J.A. (March 2020). "Angular Expansion of Nova Shells". The Astrophysical Journal. 892 (1): 60. arXiv:2002.06749. Bibcode:2020ApJ...892...60S. doi:10.3847/1538-4357/ab76c5. S2CID 211132830.
  2. ^ a b "V533 Her". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2 December 2020.
  3. ^ a b Schaefer, Bradley E. (December 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. ^ Sion, Edward M.; et al. (2017). "Far Ultraviolet Spectroscopy of Old Novae. II. RR Pic, V533 Her, and DI Lac". The Astronomical Journal. 153 (3). 109. arXiv:1701.05218. Bibcode:2017AJ....153..109S. doi:10.3847/1538-3881/153/3/109. PMC 5810142. PMID 29456254.
  5. ^ Warner, B. (February 2006). "Where have all the novae gone?". Astronomy & Geophysics. 47 (1): 29–32. Bibcode:2006A&G....47a..29W. doi:10.1111/j.1468-4004.2006.47129.x.
  6. ^ a b Haddock, F.T.; Howard, W.E. III; Malville, J.M.; Selling, T.V. (October 1963). "An Upper Limit to the 8000 Mc/S Flux Density of Nova Herculis 1963". Publications of the Astronomical Society of the Pacific. 75 (446): 456. Bibcode:1963PASP...75..456H. doi:10.1086/128005. S2CID 120169907.
  7. ^ Mayall, Margaret W. (December 1963). "Variable Star Notes". Journal of the Royal Astronomical Society of Canada. 57: 279. Bibcode:1963JRASC..57..279M.
  8. ^ McQuillin, Rachael; Evans, A.; Wilson, D.; Maxted, P.F.L.; Pollacco, D.; West, R.G.; Hounsell, R.A.; Bode, M.F. (January 2011). "Novae in the SuperWASP data base". Monthly Notices of the Royal Astronomical Society. 419 (1): 330–335. doi:10.1111/j.1365-2966.2011.19695.x. hdl:2381/11586.
  9. ^ Thorstensen, John R.; Taylor, Cynthia J. (March 2000). "Spectroscopy and orbital periods of the old novae V533 Herculis, V446 Herculis and X Serpentis". Monthly Notices of the Royal Astronomical Society. 312 (3): 629–637. Bibcode:2000MNRAS.312..629T. doi:10.1046/j.1365-8711.2000.03230.x.
  10. ^ Knigge, Christian (31 October 2006). "The donor stars of cataclysmic variables". Monthly Notices of the Royal Astronomical Society. 373 (2): 484–502. arXiv:astro-ph/0609671. Bibcode:2006MNRAS.373..484K. doi:10.1111/j.1365-2966.2006.11096.x. S2CID 2616606.
  11. ^ Gill, C.D.; O'Brien, T.J. (May 2000). "Hubble Space Telescope imaging and ground-based spectroscopy of old nova shells - I. FH Ser, V533 Her, BT Mon, DK Lac and V476 Cyg". Monthly Notices of the Royal Astronomical Society. 314 (1): 175–182. arXiv:astro-ph/0001092. Bibcode:2000MNRAS.314..175G. doi:10.1046/j.1365-8711.2000.03342.x. S2CID 119433788.
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