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Using a three-component, multi-scale diffusion model, we show that thecosmic-ray (CR) proton and helium spectra and the dipole anisotropy can beexplained with reasonable parameters. The model includes a nearby sourceassociated with the supernova remnant (SNR) that gave rise to the Gemingapulsar, a source at the Galactic center, and a component associated with theGalactic disk. The CR flux below TeV is dominated by the disk component. Thecenter source with a continuous injection of CRs starting about 18 Myr ago isneeded to explain the anisotropy above 100 TeV. With the assumption ofuniversal CR spectra injected by all SNRs, the nearby source can produce a TeVspectral bump observed at Earth via slow diffusion across the interstellarmagnetic 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 weakmagnetic turbulence with the Alfv\'{e}n Mach number $ M_{\text{A}}\approx 0.1$. Considering the modulation of the Galactic-scale anisotropy by this magneticfield, in a quasi-local approach the field may be directed at a right ascensionabout $ -90^{\circ} $ and a declination about $ -7.4^{\circ} $ in theequatorial coordinate system.

A Three-component Model for Cosmic-ray Spectrum and Dipole Anisotropy