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The extensive grid of numerical simulations of nova eruptions of Yaron etal.(2005) first predicted that some classical novae might deviate significantlyfrom the Maximum Magnitude - Rate of Decline (MMRD) relation, which purports tocharacterise novae as standard candles. Kasliwal et al. (2011) have announcedthe observational detection of an apparently new class of faint, fast classicalnovae in the Andromeda galaxy. These objects deviate strongly from the MMRDrelationship, exactly as predicted by Yaron et al. (2005). Shara et al. (2016)recently reported the first detections of faint, fast novae in M87. Thesepreviously overlooked objects are as common in the giant elliptical galaxy M87as they are in the giant spiral M31; they comprise about 40% of all classicalnova eruptions and greatly increase the observational scatter in the MMRDrelation. We use the extensive grid of nova simulations of Yaron et al. (2005)to identify the underlying causes of the existence of faint, fast novae. Theseare systems which have accreted, and can thus eject, only very low massenvelopes, of order 10^-7 - 10^-8 Msun, on massive white dwarfs. Such binariesinclude, but are not limited to, the recurrent novae. These same models predictthe existence of ultrafast novae which display decline times t2 as short asfive hours. We outline a strategy for their future detection.

astrophysical journal/the astrophysical journal

A Hubble Space Telescope Survey for Novae in M87. II. Snuffing out the  Maximum Magnitude - Rate of Decline Relation for Novae as a Non-Standard  Candle, and a Prediction of the Existence of Ultrafast Novae