MAGNETIC FIELD AMPLIFICATION IN THE THIN X-RAY RIMS OF SN 1006
https://iopscience.iop.org/article/10.1088/0004-637X/790/2/85/meta
2. CRs and cloud
kinetic model for shock particle acceleration in the presence of neutrals
A self-consistent description of shock particle acceleration in the presence of neutral hydrogen
T: Interplay between physics and geometry in Balmer filaments: the case of SN 1006
3.TEMPORAL EVOLUTION OF NON-THERMAL SPECTRA FROM SUPERNOVA REMNANTS
Assuming that supernova shocks accelerate non-thermal particles, we model the temporally evolving non-thermal particle and photon spectra at different stages in the lifetime of a standard shell-type supernova remnant (SNR).
https://iopscience.iop.org/article/10.1086/304894/pdf
4. The efficiency of the pulsar spin-down energy transfer into cosmic rays energy
0.01%–10% range of observed VHE efficiencies for other PWNe (Gallant 2007)
Gallant, Y. A. 2007, Ap&SS, 309, 197G
5.the magnetic field at the shock front is high but rapidly decays toward the inside (Pohl et al. 2005), increasing the synchrotron loss times and increasing the diffusion constant. However, the decay in magnetic field should be reflected in the radio emissivity from the forward shock to the inside,
6.evidence cosmic ray convection in galaxy NCG253
T:cosmic rays and magnetic field in the nearby starburst galaxy ngc 253
7.The interpretation of the narrow filaments as the cooling width of the multi-TeV x-ray emitting electrons implies that similar filaments are not expected in the radio observations.
T:In which shell-type SNRs should we look for gamma-rays and neutrinos from P–P collisions
8.A DECLINE IN THE NONTHERMAL X-RAY EMISSION FROM CASSIOPEIA A
https://iopscience.iop.org/article/10.1088/2041-8205/729/2/L28/pdf
see discussion discuss the variation of radio emission spectra index
9. List of snr interacting with cloud
A SYSTEMATIC SURVEY FOR BROADENED CO EMISSION TOWARD GALACTIC SUPERNOVA REMNANTS
tycho no
cas a yes
ic443 yes
10 detail of solar modulation
https://link.springer.com/content/pdf/10.1023%2FA%3A1010376901322.pdf
11. two solar minimum, ACE energy spectrum
https://openscholarship.wustl.edu/cgi/viewcontent.cgi?article=1706&context=etd
12. Near sun transport equation
In the inner heliosphere, i.e. within about 1 AU, particle propagation is influenced mainly by pitch-angle scattering and focusing. The resulting transport equation then is the focused transport equation
Space physics An Introduction to Plasmas and Particles in the Heliosphere and Magnetospheres
10 detail of solar modulation
https://link.springer.com/content/pdf/10.1023%2FA%3A1010376901322.pdf
11. two solar minimum, ACE energy spectrum
https://openscholarship.wustl.edu/cgi/viewcontent.cgi?article=1706&context=etd
12. Near sun transport equation
In the inner heliosphere, i.e. within about 1 AU, particle propagation is influenced mainly by pitch-angle scattering and focusing. The resulting transport equation then is the focused transport equation
Space physics An Introduction to Plasmas and Particles in the Heliosphere and Magnetospheres
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