PACIFIC 2014, Moorea, French Polynesia, Sep Efficient CR Acceleration and High-energy Emission at Supernova Remnants

Transcription

1 PACIFIC 2014, Moorea, French Polynesia, Sep 2014 Efficient CR Acceleration and High-energy Emission at Supernova Remnants

2 Anatomy of an SNR

3 Emission from an SNR

4 High-energy non-thermal emission = Fast-and-furious particles SNR of SN1006 Synchrotron X-rays at SNR collisionless shock >100 TeV electrons ASCA H.E.S.S. Chandra X-ray TeV γ-rays Naumann-Godo Sometimes accompanied by γ-rays There are high-energy particles! SNRs are cosmic particle accelerators! Q: What are these particles, how are they accelerated, and how much! Answers lead us to origin of Galactic CR 4

5 Particle acceleration at fast collision-less shock Particle acceleration at fast Particles scattered by magnetic 5,000 km/s near shock collision-lessturbulence shocks Diffusive Shock Acceleration (DSA) E. Fermi (elastic pitch-angle scattering) Non-linear Diffusive Shock Acceleration (NL-DSA) Theory Real story = hard problem Particles cross shock repeatedly N(E) E-2 Coupled to hydrodynamics B-field geometry (shock obliquity) CR amplifies magnetic turbulence Amplified B-field supports DSA CR escapes into ISM Wave-particle interactions D(x,p) CR e- vs ion injection/acceleration Each crossing, gain energy from DSA is nonlinear ISM: n<1cm-3 Courtesy: Y. Uchiyama shock kinetic energy ΔE/E vsk/c 1% (young SNR) e.g shock crossings Energy gain 20,000 times 1 GeV CR becomes 20 TeV Strong shocks universal power-law CR spectrum N(E) E-2 5

6 γ-ray emission mechanism

7 Origin of γ-rays from observation! Characteristic shape of γ-ray spectrum GeV and radio bright No synchrotron X-ray 1720MHz OH masers and IR lines Shocks in molecular and atomic clouds π 0 -decay origin of γ-rays CR ion acceleration confirmed! Center-filled thermal X-ray not related to non-thermal emission from shell Mechanism of CR ion acceleration unclear Slow cloud shock Fast Coulomb energy loss Origin of energy break of CR spectra

8 Origin of γ-rays from observation SNR RX J ! Matching shape of X-ray and TeV γ-ray T. Tanaka Same origin of γ-ray and X-ray (from CR e - )? Hard γ-ray spectrum inverse Compton? Non-detected thermal X-ray low density Leptonic scenario for γ-ray origin is natural but, not so fast HL

9 Reality: often not black or white A similar SNR RX J (Vela Jr.) Sign of shock-cloud interaction! Regions of contrast seen between X and TeV

10 Time evolution of γ-ray Different progenitors and CSM involved Unified evolution picture requires careful modeling of each type of SNR! 10

11 CR Acceleration at SNRs Numerical Approaches

12 1-D Model Infrastructure

13 Iterative Work Flow

14 Non-linear Diffusive Shock Acceleration! e.g. HL, Ellison & Nagataki (2012) Thermal distribution CR spectrum at forward shock e- p Spectra at different locations in precursor Adiabatic Coulomb loss Synch loss

15 Application to young SNRs

16 Application to Middle-aged SNRs with Radiative Shocks

17 Nonlinear Diffusive Shock Acceleration with wave-particle interactions

18 Thermal X-rays TFe log(temperature [K]) Tp Te TFe log(ion fraction) Te Time Si XIII Si XII RS R [RRS] CD

19 Powerful constraint of γ-ray origin Thermal X-ray

20 Synthesis of detailed X-ray spectra

21 Multi-D Hydro-NEI Simulation of SNRs Path towards connecting SNe and SNRs!

22 Ultimate Research Goal From engine to remnant, and back T. Takiwaki >>> >>> <<< <<< D. Warren Engine Remnant In computers Cas A, LAT, Chandra What s out there Iteration between improving models and observations > full understanding of last stage of stellar evolution

23 Roadmap

24 Summary from engine to remnant