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Recent measurements of primary and secondary CR spectra, their arrivaldirections, and our improved knowledge of the magnetic field geometry aroundthe heliosphere allow us to set a bound on the distance beyond which a puzzling10-TeV "bump" cannot originate. The sharpness of the spectral breaks associatedwith the bump, the abrupt change of the CR intensity across the local magneticequator ($90^{\circ}$ pitch angle), and the similarity between the primary andsecondary CR spectral patterns point to a local reacceleration of the bumpparticles out of the background CRs. We argue that a nearby shock may generatesuch a bump by increasing the rigidity of the preexisting CRs below 50 TV by amere factor of ~1.5. Reaccelerated particles below ~0.5 TV are convected withthe interstellar medium flow and do not reach the Sun, thus creating the bump.This single universal process is responsible for the observed spectra of all CRspecies in the rigidity range below 100 TV. We propose that one viablecandidate is the system of shocks associated with Epsilon Eridani star at 3.2pc of the Sun, which is well aligned with the direction of the local magneticfield. Other shocks, such as old supernova shells, may produce a similareffect. We provide a simple formula that reproduces the spectra of all CRspecies with only three parameters uniquely derived from the CR proton data. Weshow how our formalism predicts helium and carbon spectra and the B/C ratio.

On Why the 10-TeV Cosmic Ray Bump Originates in the Local Interstellar Medium