On the origin of observed cosmic ray spectrum below 100 TV. (arXiv:2105.04630v2 [astro-ph.HE] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Malkov_M/0/1/0/all/0/1">Mikhail A. Malkov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moskalenko_I/0/1/0/all/0/1">Igor V. Moskalenko</a>

Recent precise measurements of primary and secondary cosmic rays (CRs) in the
TV rigidity domain have unveiled a bump in their spectra, located between
0.5-50 TV. We argue that a local shock may generate such a bump by increasing
the rigidity of the preexisting CRs below 50 TV by a mere factor of ~1.5.
Reaccelerated particles below ~0.5 TV are convected with the interstellar
medium (ISM) flow and do not reach the Sun, thus creating the bump. This single
universal process is responsible for the observed spectra of all CR species in
the rigidity range below 100 TV. We propose that one viable shock candidate is
the Epsilon Eridani star at 3.2 pc from the Sun, which is well-aligned with the
direction of the local magnetic field. Other shocks, such as old supernova
shells, may produce a similar effect. We provide a simple formula, Eq. (9),
that reproduces the spectra of all CR species with only two nonadjustable shock
parameters, uniquely derived from the proton data. We show how our formalism
predicts helium and carbon spectra and the B/C ratio.

Recent precise measurements of primary and secondary cosmic rays (CRs) in the
TV rigidity domain have unveiled a bump in their spectra, located between
0.5-50 TV. We argue that a local shock may generate such a bump by increasing
the rigidity of the preexisting CRs below 50 TV by a mere factor of ~1.5.
Reaccelerated particles below ~0.5 TV are convected with the interstellar
medium (ISM) flow and do not reach the Sun, thus creating the bump. This single
universal process is responsible for the observed spectra of all CR species in
the rigidity range below 100 TV. We propose that one viable shock candidate is
the Epsilon Eridani star at 3.2 pc from the Sun, which is well-aligned with the
direction of the local magnetic field. Other shocks, such as old supernova
shells, may produce a similar effect. We provide a simple formula, Eq. (9),
that reproduces the spectra of all CR species with only two nonadjustable shock
parameters, uniquely derived from the proton data. We show how our formalism
predicts helium and carbon spectra and the B/C ratio.

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