  Measurements of cosmic rays by experiments such as ATIC, CREAM, and PAMELA
indicate a hardening of the cosmic-ray energy spectrum at TeV energies. In our
recent work (Thoudam & H\"orandel 2012a), we showed that the hardening can be
due to the effect of nearby supernova remnants. We showed it for the case of
proton and helium. In this paper, we present an improved and detailed version
of our previous work, and extend our study to heavier cosmic-ray species such
as boron, carbon, oxygen, and iron nuclei. Unlike our previous study, the
present work involves a detailed calculation of the background cosmic rays and
follows a consistent treatment of cosmic-ray source parameters between the
background and the nearby components. Moreover, we also present a detailed
comparison of our results on the secondary-to-primary ratios, secondary
spectra, and the diffuse gamma-ray spectrum with the results expected from
other existing models, which can be checked by future measurements at high
energies.
