Stochastic Acceleration of Cosmic Rays in the Central Molecular Zone of the Galaxy
arXiv:1110.3140 · doi:10.1093/pasj/63.6.L63
Abstract
Particle acceleration in the inner ~ 200 pc of the Galaxy is discussed, where diffuse TeV gamma-rays have been detected by the High Energy Stereoscopic System (HESS) observation. The diffuse gamma-ray emission has a strong correlation with molecular clouds with large velocity dispersion, indicating the presence of turbulence. It is argued that the turbulence may contribute to the acceleration of cosmic rays via stochastic acceleration. The stochastic acceleration may energize cosmic-ray protons up to ~ 100 TeV and electrons to ~ 1 TeV in a relatively tenuous medium. The difference in the efficiency between protons and electrons supports the hadronic scenario of the diffuse TeV gamma-ray emission.
4 pages, 1 figure, accepted by PASJ Letters
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Cited by in corpus (7)
- Observational signatures of particle acceleration in supernova remnants
- Non-Thermal Insights on Mass and Energy Flows Through the Galactic Centre and into the Fermi Bubbles
- Gamma rays from the Galactic Centre region: a review
- Espresso and Stochastic Acceleration of Ultra-high-energy Cosmic Rays in Relativistic Jets
- Hadronic origin of multi-TeV gamma rays and neutrinos from low-luminosity active galactic nuclei: implications of past activities of the Galactic center
- Cosmic-Ray Models of the Ridge-Like Excess of Gamma Rays in the Galactic Center
- Molecular and Atomic Gas toward HESS J1745-303 in the Galactic Center: Further Support for the Hadronic Scenario