  Growing evidence reveals universal hardening on various cosmic ray spectra,
e.g. proton, positron, as well as antiproton fraction. Such universality may
indicate they have a common origin. In this paper, we argue that these
widespread excesses can be accounted for by a nearby supernova remnant
surrounded by a giant molecular cloud. Secondary cosmic rays ($\rm p$, $\rm
e^+$) are produced through the collisions between the primary cosmic ray nuclei
from this supernova remnant and the molecular gas. Different from the
background, which is produced by the ensemble of large amount of sources in the
Milky Way, the local injected spectrum can be harder. The time-dependent
transport of particles would make the propagated spectrum even harder. Under
this scenario, the anomalies of both primary ($\rm p$, $\rm e^-$) and secondary
($\rm e^+$, $\rm \bar{p}/p$) cosmic rays can be properly interpreted. We
further show that the TeV to sub-PeV anisotropy of proton is consistent with
the observations if the local source is relatively young and lying at the
anti-Galactic center direction.
