Understanding the galactic cosmic ray dipole anisotropy with a nearby single source under the spatially-dependent propagation scenario. (arXiv:1901.00249v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Qu_X/0/1/0/all/0/1">Xiaobo Qu</a>
Recently studies of the dipole anisotropy in the arrival directions of
Galactic cosmic rays indicate that the TeV-PeV dipole anisotropy amplitude is
not described by a simple power law, moreover a rapid phase change exists at an
energy of $0.1sim0.3$ PeV. In this work we argue that the dipole anisotropy
amplitude and phase evolution with energies can be reproduced under the
spatially-dependent propagation scenario with a nearby single source added. Our
results indicate a nearby single source have significant influence to the
cosmic ray gradient below $0.1sim0.3$ PeV under the spatially-dependent
propagation scenario, which leads the dipole anisotropy phase change at this
energy region. The dipole anisotropy amplitude of the galactic cosmic rays can
also be maintained at a lower level, which are consistent with observations by
underground muons and air shower experiments.
Recently studies of the dipole anisotropy in the arrival directions of
Galactic cosmic rays indicate that the TeV-PeV dipole anisotropy amplitude is
not described by a simple power law, moreover a rapid phase change exists at an
energy of $0.1sim0.3$ PeV. In this work we argue that the dipole anisotropy
amplitude and phase evolution with energies can be reproduced under the
spatially-dependent propagation scenario with a nearby single source added. Our
results indicate a nearby single source have significant influence to the
cosmic ray gradient below $0.1sim0.3$ PeV under the spatially-dependent
propagation scenario, which leads the dipole anisotropy phase change at this
energy region. The dipole anisotropy amplitude of the galactic cosmic rays can
also be maintained at a lower level, which are consistent with observations by
underground muons and air shower experiments.
http://arxiv.org/icons/sfx.gif
