Nova that appeared in 1936
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! style="text-align: center; background-color: #FFFFC0;" colspan="2" | Observation dataEpoch J2000.0      Equinox J2000.0
! style="text-align:left" | Constellation
! style="text-align:left" | Right ascension
! style="text-align:left" | Declination
! style="text-align:left" | Apparent magnitude (V)
! style="background-color: #FFFFC0; text-align: center;" colspan="2"| Characteristics
! style="text-align:left" | Variable type
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V630 Sagittarii (Nova Sagittarii 1936) was a nova visible to the naked eye in 1936. It was discovered on 3 October 1936 by Shigeki Okabayashi of Kobe, Japan when it had an apparent magnitude of 4.5.
There is disagreement within the astronomical literature about what this nova's peak brightness was. Both Warner and Downes "et al." report a peak brightness of magnitude 1.6 but Duerbeck reports 4.0 in rough agreement with the Harrison and Gehrz value of 4.5. The AAVSO database contains no magnitude estimates for this star brighter than 6.5 (on 8 October 1936), indicating that whatever the peak brightness was, the star was barely visible to the naked eye just five days after its discovery. Its light curve shows it to be one of the most rapidly fading novae on record.
Duerbeck estimated that the star's absolute magnitude at peak brightness was −9.3. Diaz and Steiner list it as a possible magnetic nova, due to its short decay time ( ; 20 days) and large amplitude outburst.
All classical novae are binary systems, with a donor star losing mass onto the surface of a white dwarf. Mróz "et al." report that in the case of V630 Sagittarii, the donor star is a main sequence star. Since all classical novae are very close binary systems, they are frequently also eclipsing binaries. Woudt and Warner detected these eclipses, which are 0.4 to 0.6 magnitudes deep, allowing them to derive an orbital period of 2.831 hours. Mróz "et al." report the presence of superhumps.
References.
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