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The nature of an emerging class of rapidly fading supernovae(RFSNe)--characterized by their short-lived light curve duration, but varyingwidely in peak brightness--remains puzzling. Whether the RFSNe arise fromlow-mass thermonuclear eruptions on white dwarfs or from the core collapse ofmassive stars is still a matter of dispute. We explore the possibility that theexplosion of hydrogen-free massive stars could produce bright but rapidlyfading transients if the effective pre-supernova radii are large and if littleor no radioactive nickel is ejected. The source of radiation is then purely dueto shock cooling. We study this model of RFSNe using spherically symmetrichydrodynamics and radiation transport calculations of the explosion of strippedstars embedded in helium-dominated winds or shells of various masses andextent. We present a parameter study showing how the properties of thecircumstellar envelopes affect the dynamics of the explosion and can lead to adiversity of light curves. We also explore the dynamics of the fallback of theinnermost stellar layers, which might be able to remove radioactive nickel fromthe ejecta, making the rapid decline in the late time light curve possible. Weprovide scaling relations that describe how the duration and luminosity ofthese events depend on the supernova kinetic energy and the mass and radius ofthe circumstellar material.

Models of bright nickel-free supernovae from stripped massive stars with circumstellar shells