A Galactic Cosmic Ray Electron Spectrum from 2 MeV to 2 TeV That Fits Voyager 5-60 MeV Data at Low Energies and PAMELA and AMS-2 Data at 10 GeV Using an Electron Source Spectrum E^-2.25 A Calculation Using a Monte Carlo Diffusion Model
In this paper we fit the observed galactic cosmic ray electron spectrum from a few MeV to 1 TeV. New data from Voyager from 5-60 MeV beyond the heliopause is used along with high energy data from the PAMELA, FERMI and AMS-2 instruments in Earth orbit. Using a Monte Carlo diffusion model for galactic propagation we obtain a source rigidity spectrum with a spectral index =-2.25 independent of energy below 10 GeV, possibly steepening above 10 GeV to 2.40 at the highest energies. This spectrum will fit the electron data over 5 orders of magnitude to within + 10% at both low and high energies. This steepening of the electron source spectrum could be an important feature of the acceleration process, e.g., synchrotron loss during acceleration could steepen the source spectrum. This fit requires only a single break in the rigidity dependence of the diffusion coefficient by ~1.0 power in the exponent at about 1.0 GV. The calculations also predict the distribution of electrons perpendicular to the galactic disk. The galaxy does act as a calorimeter for electrons in the energy range 0.1-10 GeV where ~80% of the electrons are trapped. At higher energies the electrons escape the galactic disk rapidly. At energies ~1 TEV the electrons loose most of their energy by synchrotron and inverse Compton emission within < 0.5 Kpc of their origin near the galactic equator. At energies < 0.1 GeV, because of the increase in the diffusion coefficient below ~1 GV, and the absence of other significant loss processes, the electrons escape and form a difficult to detect, but important galactic halo population.
Determination of the Total Solar Modulation Factors in the Heliosphere For Cosmic Ray Protons and Electrons by Comparing Interstellar Spectra Deduced from Voyager Measurements and PAMELA Spectra of These Particles at the Earth
Calculations of the Propagated LIS Electron Spectrum Which Describe the Cosmic Ray Electron Spectrum below ~100 MeV Measured Beyond 122 AU at Voyager 1 and its Relationship to the PAMELA Electron Spectrum above 200 MeV
新的旅行者测量宇宙射线电子之间的6-60兆电子伏超过122 AU是非常敏感的指标宇宙射线传播和加速在星系中在一个非常低的调制水平。使用蒙特卡罗扩散模型与源光谱与一个单一的光谱指数为-2.2在所有的能量，我们能够适应这个观察到的旅行者光谱和当代PAMELA电子光谱的能量范围从6 MeV到~200 GeV。这个频谱中有一个中断，但这个中断是由于传播效应，而不是主频谱的变化。这种突变是逐渐发生的，从能量大于2 GeV的能量开始，此时的能谱为~E^-3.2，然后继续下降到能量小于或等于100 MeV的能量，此时的能谱为~E^-1.5。在较高的能量下，由于同步辐射和逆康普顿效应产生的损失项约为E^2.0，使源谱的指数变陡1.0。在较低的能量下，这些项变得不重要，损失由扩散和逃离星系决定。在~0.32 GV以下，扩散项与β ^-1成正比（这也符合在旅行者号上测得的氢和氦的光谱），在1 GV时的值为3 × 1028 cm ^2 x s^-1，边界在+/-1 Kpc，这将符合旅行者号或其他类似的低能光谱。
Fitting the Galactic Electron Spectrum Measured by Voyager at Low Energies and also by CALET/AMS-2 at High Energies Using a Monte Carlo Diffusion Model for Electron Propagation - One Spectrum Fits All
The Galactic Cosmic Ray Electron Spectrum from 3 to 70 MeV Measured by Voyager 1 Beyond the Heliopause, What This Tells Us About the Propagation of Electrons and Nuclei In and Out of the Galaxy at Low Energies
A Comparison of Galactic Cosmic Ray Proton and Helium Nuclei Spectra From ~10 MeV/nuc to 1 TeV/nuc Using New Voyager and Higher Energy Magnetic Spectrometer Measurements - Are There Differences In the Source Spectra of The Two Nuclei
The Separation of Secondary Positrons Produced in the Galaxy from the High Energy Positrons that are Observed Recent Space Experiments on PAMELA and AMS2
A Study of the B/C Ratio Between 10 MeV/nuc and 1 TeV/nuc in Cosmic Rays Using New Voyager and AMS-2 Data and a Comparison with the Predictions of Leaky Box Propagation Models
The Cosmic Ray Helium and Carbon Nuclei Spectra Measured by Voyager 1 at Low Energies and Earth Based Measurements of these Nuclei up to 200 GeV nuc Concordance at High Energies with a Leaky Box Propagation Model
A Fit to the Galactic Cosmic Ray Hydrogen and Helium Spectra at Voyager 1 at Low Energies and Earth Based Measurements at Much Higher Energies with Identical Rigidity Independent Source Spectra for the Hydrogen and Helium Nuclei
A Comparison of the Galactic Cosmic Ray Electron and Proton Intensities From 1 MeV/nuc to 1 TeV/nuc Using Voyager and Higher Energy Magnetic Spectrometer Measurements Are There Differences in the Source Spectra of These Particles?
A Comparison of the Galactic Cosmic Ray H, He and C/O Nuclei Spectra Measured Between ~5 and 500 MeV/nuc Beyond 122 AU at Voyager 1 with the Predictions of a Diffusion Model for Propagation in the Galaxy
Interstellar Spectra of Primary Cosmic Ray Nuclei from H through Fe Measured at Voyager and a Comparison with Higher Energy Measurements, An Interpretation of the Spectra from 10 MeVnuc to Over 100 GeVnuc Using a Leaky Box Model
The Different Shapes of the LIS Energy Spectra of Cosmic Ray He and C Nuclei Below ~1 GeV/nuc and The Cosmic Ray He/C Nuclei Ratio vs. Energy -V1 Measurements and LBM Propagation Predictions
