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We present multi-wavelength observations of SN2014C during the first 500days. These observations represent the first solid detection of a youngextragalactic stripped-envelope SN out to high-energy X-rays. SN2014C was theexplosion of an H-stripped progenitor star with ordinary explosion parameters.However, over the time scale of ~1yr, SN2014C experienced a completemetamorphosis and evolved from an ordinary H-poor supernova of type Ib into astrongly interacting, H-rich supernova of type IIn. Signatures of the SN shockinteracting with a dense medium are observed across the spectrum. Coordinatedobservations with Swift, Chandra and NuSTAR have captured the evolution indetail and revealed the presence of a massive shell of ~1 Msun of hydrogen-richmaterial at ~6d16 cm from the explosion site. We estimate that the shell wasejected by the progenitor star in the decades to centuries before corecollapse. This result poses significant challenges to current theories ofmassive star evolution, as it requires a physical mechanism responsible for theejection of the deepest hydrogen layer of H-poor SN progenitors synchronizedwith the onset of stellar collapse. Theoretical investigations point at binaryinteractions and/or instabilities during the last stages of nuclear burning inmassive stars as potential triggers of the time-dependent mass loss. Weconstrain these scenarios utilizing the sample of 183 SNe Ib/c with publicradio observations. Our analysis identifies SN2014C-like signatures in ~10% ofSNe with constraining radio data. This fraction is somewhat larger butreasonably consistent with the expectation from the theory of recent envelopeejection due to binary evolution IF the ejected material can survive in theclose environment for 1000-10000 yrs. Alternatively, nuclear burninginstabilities extending all the way to the core C-burning phase might also playa critical role.

Ejection of the massive Hydrogen-rich envelope timed with the collapse of the stripped SN2014C