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A class of very energetic supernovae (hypernovae) is associated with longgamma-ray bursts, in particular with a less energetic but more frequentpopulation of gamma-ray bursts. Hypernovae also appear to be associated withmildly relativistic jets or outflows, even in the absence of gamma-ray bursts.Here we consider radiation from charged particles accelerated in such mildlyrelativistic outflows with kinetic energies of ~10^{50} erg. The radiationprocesses of the primarily accelerated electrons considered are synchrotronradiation and inverse-Compton scattering of synchrotron photons (synchrotronself-Compton; SSC) and of supernova photons (external inverse-Compton; EIC). Inthe soft X-ray regime, both the SSC and EIC flux can be the dominant component,but due to their very different spectral shapes it should be easy todistinguish between them. When the fraction of the kinetic energy going intothe electrons (\epsilon_e) is large, the SSC is expected to be important;otherwise the EIC will dominate. The EIC flux is quite high, almostindependently of \epsilon_e, providing a good target for X-ray telescopes suchas XMM-Newton and Chandra. In the GeV gamma-ray regime, the EIC would be thedominant radiation process and the Gamma-ray Large Area Space Telescope (GLAST)should be able to probe the value of \epsilon_e, the spectrum of the electrons,and their maximum acceleration energy. Accelerated protons also lead to photonradiation through the secondary electrons produced by the photopion andphotopair processes. We find that over a significant range of parameters theproton component is generally less prominent than the primary electroncomponent. We discuss the prospects for the detection of the X-ray and GeVsignatures of the mildly relativistic outflow of hypernovae.

Broadband Radiation from Primary Electrons in Very Energetic Supernovae