  Using a three-component, multi-scale diffusion model, we show that the
cosmic-ray (CR) proton and helium spectra and the dipole anisotropy can be
explained with reasonable parameters. The model includes a nearby source
associated with the supernova remnant (SNR) that gave rise to the Geminga
pulsar, a source at the Galactic center, and a component associated with the
Galactic disk. The CR flux below TeV is dominated by the disk component. The
center source with a continuous injection of CRs starting about 18 Myr ago is
needed to explain the anisotropy above 100 TeV. With the assumption of
universal CR spectra injected by all SNRs, the nearby source can produce a TeV
spectral bump observed at Earth via slow diffusion across the interstellar
magnetic field, which needs to have an angle $ \theta \approx 5^{\circ} $
between the field line and the line of sight toward the source, and have weak
magnetic turbulence with the Alfv\'{e}n Mach number $ M_{\text{A}}\approx 0.1
$. Considering the modulation of the Galactic-scale anisotropy by this magnetic
field, in a quasi-local approach the field may be directed at a right ascension
about $ -90^{\circ} $ and a declination about $ -7.4^{\circ} $ in the
equatorial coordinate system.
