Recent observations found that electrons are accelerated to ~10 GeV and emit synchrotron
hard X-rays in two magnetic white dwarfs (WDs), also known as cataclysmic variables (CVs).
In nova outbursts of WDs, multi-GeV gamma-rays were detected inferring that protons are
accelerated to 100 GeV or higher. In recent optical surveys, the WD density is found to be
higher near the Sun than in the Galactic disk by a factor ~2.5. The cosmic rays (CR) produced
by local CVs and novae will accumulate in the local bubble for 10^6-10^7 yrs. On these findings,
we search for CRs from historic CVs and novae in the observed CR spectra. We model the CR
spectra at the heliopause as sums of Galactic and local components based on observational
data as much as possible. The initial Galactic CR electron and proton spectra are deduced
from the gamma-ray emissivity, the local electron spectrum from the hard X-ray spectra at
the CVs, and the local proton spectrum inferred by gamma-ray spectrum at novae. These
spectral shapes are then expressed in a simple set of polynomial functions of CR energy and
regressively fitted until the high-energy (>100 GeV) CR spectra near Earth and the Voyager-1
spectra at the heliopause are reproduced. We then extend the modeling to nuclear CR spectra
and find that one spectral shape fits all local nuclear CRs and the apparent hardening of the
nuclear CR spectra is caused by the roll-down of local nuclear spectra around 100-200 GeV.
All local CR spectra populate in a limited energy band below 100-200 GeV and enhance
gamma-ray emissivity below ~10 GeV. Such an enhancement is observed in the inner Galaxy,
suggesting the CR fluxes from CVs and novae are substantially higher there.