The light curve of V368 Aql, plotted from data presented by Parenago.[4] The red points are visible light magnitudes, and the blue points are photographic magnitudes.
V368 Aquilae, also known as Nova Aquilae 1936 no. 2 was the second
Hα emission, and for a time could be seen with binoculars simultaneously with V356 Aquilae, another nova which Nill Tamm had discovered a month earlier.[8]
V368 Aquilae is classified as a "moderately fast nova"; it dropped by three magnitudes in about 42 days.[9]
All novae are binary stars, with a "donor" star orbiting a white dwarf. The two stars are so close to each other that matter is transferred from the donor star to the white dwarf. Because the separation between the stars is comparable to the size of the donor star, these stars are often eclipsing binaries and V368 Aquilae does show eclipses. Marin and Shfter studied these eclipses, which have a depth of about 0.25 magnitudes and a period of 16.57 hours - an unusually long orbital period for a nova.[9]
