Origin of the spectral features observed in the cosmic-ray spectrum

被引:3
作者
Recchia, S. [1 ,2 ,3 ]
Gabici, S. [4 ]
机构
[1] INAF Osservatorio Astron Brera, Via Bianchi 46, I-23807 Merate, Italy
[2] Univ Torino, Dipartimento Fis, Via P Giuria 1, I-10125 Turin, Italy
[3] Ist Nazl Fis Nucleare, Sez Torino, Via P Giuria 1, I-10125 Turin, Italy
[4] Univ Paris Cite, CNRS, AstroParticule & Cosmol, F-75013 Paris, France
关键词
diffusion; cosmic rays; Galaxy: disk; Galaxy: halo; ENERGY-SPECTRA; SUPERNOVA-REMNANTS; NUCLEI; DIFFUSION; ACCELERATION; PROPAGATION; TURBULENCE; TRANSPORT; SIMULATIONS; CONSTRAIN;
D O I
10.1051/0004-6361/202349005
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Context. Recent measurements reveal the presence of several features in the cosmic-ray (CR) spectrum. In particular, the proton and helium spectra exhibit a spectral hardening at approximate to 300 GV and a spectral steepening at approximate to 15 TV, followed by the well-known knee-like feature at approximate to 3 PV. The spectra of heavier nuclei also harden at approximate to 300 GV, while no claim can be currently made about the presence of the approximate to 15 TV softening, due to low statistics. In addition, the B/C ratio also exhibits a hardening at approximate to 100 GeV/n and seems to be rather shallow at approximate to 1 TeV/n Aims. We propose a possible explanation of the observed spectral features in the framework of a composite diffusion scenario and considering different classes of sources. Methods. The proposed scenario is based 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 CRs 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 approximate to 15 TV is related to the typical maximum rigidity reached in the acceleration of CRs by the majority of supernova remnants, while we assume that only a fraction of sources, contributing to approximate to 10 - 20% of the CR population, can accelerate particles up to similar to PV rigidities. Results. Within this framework we show that it is possible to reproduce the proton and helium spectra from GV to multi-PV; the p/He ratio; the spectra of CRs from lithium to iron; the (p) over bar flux and the (p) over bar /p ratio; and the abundance ratios B/C, B/O, C/O, Be/C, Be/O, and Be/B. We also discuss the Be-10/Be-9 ratio in view of the recent AMS02 preliminary measurements.
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