Cosmic-ray acceleration by forward and reverse shocks in young SNR

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Presentation transcript:

Cosmic-ray acceleration by forward and reverse shocks in young SNR Martin Pohl U-Potsdam and DESY Zeuthen with Igor Telezhinsky and Vikram Dwarkadas

Modelling methods Gas hydro with semi-analytical acceleration Gas hydro + CR acceleration and transport Full account of gas, CRs, and MF only plane-parallel shock, no transport can include CR feedback accurate CR transport multiple shocks possible CR feedback difficult maybe at ICRC 2013 ...

Hydrodynamical profiles Often assumed: Sedov phase Late time only!

Reality: dynamical evolution Typically at least 2 shocks! Acceleration everywhere, because

The method 1. Use flow profiles from hydrodynamical simulations 2. Solve CR transport equation for these flow profiles. Advantage: Accurate treatment of acceleration and transport Consistent account of escape possible Disadvantage: No account for CR feedback (works for low CR pressure)

The method Transformation of spatial coordinate required Diffusion coefficient can be coupled to MF profile 2 MF profiles used thus far D: density scaling P: pressure scaling 4. Multiple shocks can be accounted for 5. Self-consistent calculation of emission

Magnetic-field profiles Examples of MF profiles for Type 1a Magnetic-field amplification at shocks M1: Caprioli et al. 2009 M2: constant amplification factor More accurate MF transport forthcoming

Particle spectra Note the bumps in the spectra! Electrons Protons Here density scaling of MF with 75 mG at forward shock Note the bumps in the spectra!

It is critical to know where gas and MF sits Emission (Type 1a) It is critical to know where gas and MF sits

With more MF amplification Electrons Protons Again density scaling, but relative to Caprioli model at forward shock

Emission (Type 1a)

Surface Brightness Maps M1 M2 RADIO 1.4GHz SY 3 keV PD 1 TeV IC 1 TeV

Conclusions Realistic fluid profiles are important for modeling Reverse shock can dominate for young SNR Adiabatic cooling/heating throughout the system Complicated particle / emission spectra Hard gamma-ray spectra don‘t always imply CR modification