1. energy equipartition to determine the magnetic field
2. derive the parker equation and adiabatic energy loss
https://indico.cern.ch/event/656460/contributions/2679912/attachments/1686296/2711748/TPE-handout.pdf
ON THE EQUATION OF TRANSPORT FOR COSMIC-RAY PARTICLES IN THE INTERPLANETARY REGION
ON THE EQUATION OF TRANSPORT FOR COSMIC-RAY PARTICLES IN THE INTERPLANETARY REGION
adiabatic
cooling
3. different description on the parker eq: distribution function vs number density
| Cosmic Rays in the Interplanetary Radiation Environments and Damage in Silicon Semiconductors Silicon |
4. Cosmic ray astrophysics (history and general review)
5.Cosmic-ray acceleration and transport, and diffuse galactic gamma-ray emission
http://adsabs.harvard.edu/abs/1983SSRv...36....3V
6. introduction to turbulence
http://www.astronomy.ohio-state.edu/~ryden/ast825/ch7.pdf
7. review of cosmic ray physics
8.Magnetic fields in supernova remnants and pulsar-wind nebulae
https://arxiv.org/pdf/1104.4047.pdf
9. particle trajectory in magnetic field
Revisiting the Equipartition Assumption in Star-forming Galaxies
10. MF review
Practical Modeling of Large-Scale Galactic MagneticFields: Status and Prospects
11. electron spectrum in SNR
Analytical solutions for energy spectra of electrons accelerated by nonrelativistic shock-waves in shell type supernova remnants
COSMIC-RAY ELECTRON EVOLUTION IN THE SUPERNOVA REMNANT RX J1713.7–3946
Evolution of cosmic ray electron spectra in magnetohydrodynamical simulations
12. sun magnetic field 11 evolution
http://www.astrophys-space-sci-trans.net/4/19/2008/astra-4-19-2008.pdf
13. More detailed Monte Carlo models of shock acceleration that include the nonlinear e†ects of the accelerated particles on the shock itself (Ellison et al. 1995, 1996) produce somewhat di†erent results. For the same overall compression ratio, the particle spectra at nonrelativistic energies tend to have spectral indices steeper than that given by the simple model discussed above (2.5), while at ultrarelativistic energies, the spectra Ñatten to indices somewhat less than discussed above (1.5).
https://iopscience.iop.org/article/10.1086/304894/pdf
14.
Radio Properties of Pulsar Wind Nebulae
https://link.springer.com/chapter/10.1007%2F978-3-319-63031-1_1
15. radio index in snr
https://arxiv.org/pdf/1907.00966.pdf
15. introduction to CR
http://astro.tsinghua.edu.cn/~xbai/teaching/PlasmaCourse2016/Ay253_2016_12_CosmicRays.pdf
16. CR escape
https://arxiv.org/pdf/1801.08890.pdf
17. Protheroe (2004) performed a detailed study of the shape of the
cutoff for particles experiencing diffusive shock acceleration
18. Diffusive Shock Acceleration and Magnetic Field Amplification
15. radio index in snr
https://arxiv.org/pdf/1907.00966.pdf
15. introduction to CR
http://astro.tsinghua.edu.cn/~xbai/teaching/PlasmaCourse2016/Ay253_2016_12_CosmicRays.pdf
16. CR escape
https://arxiv.org/pdf/1801.08890.pdf
18. Diffusive Shock Acceleration and Magnetic Field Amplification
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