Cosmic-Ray proton spectrum below 100 TeV in the local region
arXiv:astro-ph/0604535 · doi:10.1111/j.1365-2966.2006.10456.x
Abstract
The propagation of cosmic-ray protons in the Galaxy is discussed under the framework of a three dimensional convection-diffusion model. Starting with the assumption of a uniform and continuous distribution of cosmic-ray sources injecting CRs continuously in the Galaxy and by invoking a supernova explosion at various distances from the Earth, it is found that only those sources located within a distance of ~ 1.5 kpc can produce appreciable temporal fluctuations in the CR proton flux observed at the Earth. So, the construction of the local CR proton spectrum is discussed by seperating the contributions of the distant sources from that of the nearby sources. The contribution from the distant sources is treated in the framework of a continuous source distribution model both in space as well as time, but that of the nearby sources in a discrete space-time source model. The study predicts the presence of at least one old nearby source with a characteristic age of ~ 10^5 yrs located at a distance of ~ 0.1 kpc to explain the observed proton flux below ~ 100 GeV.
arXiv comment8 pages, 6 figures, 1 table, uses mn2e.cls, minor text corrections, accepted for publication in MNRAS
References in corpus (8)
- X-Ray Emission From the Shell-Type SNR G347.3-0.5
- Discovery of Non Thermal X-Rays from the Northwest Shell of the New SNR RX J1713.7-3946: The Second SN1006 ?
- The Most Likely Sources of High Energy Cosmic-Ray Electrons in Supernova Remnants
- RXJ 0852.0-0462: Another Nonthermal Shell-Type SNR (G266.2-1.2)
- Evidence of X-ray Synchrotron Emission from Electrons Accelerated to 40 TeV in the Supernova Remnant Cassiopeia A
- Emission of SN 1006 produced by accelerated cosmic rays
- A Possible Site of Cosmic Ray Acceleration in the Supernova Remnant IC 443
- The Search for the Sidereal and Solar Diurnal Modulations in the Total MACRO Muon Data Set