  Recent measurements revealed the presence of several features in the cosmic
ray spectrum. In particular, the proton and helium spectra exhibit a spectral
hardening at $\approx$ 300 GV and a spectral steeping at $\approx$ 15 TV,
followed by the well known knee-likefeature at $\approx$ 3 TV. The spectra of
heavier nuclei also harden at $\approx$ 300 GV, while no claim can be currently
done about the presence of the $\approx$ 15 TV softening, due to low
statistics. In addition, the B/C ratio flattens at $\approx$ 1 TeV/n. We
present a novel scenario for cosmic ray sources and transport in the Galaxy
that may explain all of the observed spectral features. The proposed scenario
is based mainly on two assumptions. First, in the Galactic disk, where magnetic
field lines are mainly oriented along the Galactic plane, particle scattering
is assumed to be very inefficient. Therefore, the transport of cosmic rays from
the disk to the halo is set by the magnetic field line random walk induced by
large scale turbulence. Second, we propose that the spectral steepening at
$\approx$ 15 TV is related to the typical maximum rigidity reached in the
acceleration of cosmic rays by the majority of supernova remnants, while we
assume that only a fraction of sources, contributing to $\approx$ 10-20% of the
cosmic ray population, can accelerate particles up to $\sim$ PV. We show that,
within this framework, it is possible to reproduce the proton and helium
spectra from GV to multi-PV, and the p/He ratio, the spectra of cosmic ray from
lithium to iron, the $\bar{p}$ flux and the $\bar{p}$/p ratio and the abundance
ratios B/C, B/O, C/O, Be/C, Be/O, Be/B. We also discuss the $^{10}$Be/ $ ^9$Be
ratio in view of the recent AMS02 preliminary measurements.
