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A CR-HYDRO-NEI MODEL OF STRUCTURE AND BROADBAND EMISSION FROM TYCHO’S SNR Slane et al.

Zhang Ningxiao. A CR-HYDRO-NEI MODEL OF STRUCTURE AND BROADBAND EMISSION FROM TYCHO’S SNR Slane et al. . Warren et al. 2005. Emission of Tycho from Radio to γ -ray. The γ -ray is mainly accelerated from hadronic processes. BACKGROUND. π 0-decay Inverse compton (IC)

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A CR-HYDRO-NEI MODEL OF STRUCTURE AND BROADBAND EMISSION FROM TYCHO’S SNR Slane et al.

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  1. Zhang Ningxiao A CR-HYDRO-NEI MODEL OF STRUCTURE AND BROADBAND EMISSION FROM TYCHO’S SNRSlane et al.

  2. Warren et al. 2005

  3. Emission of Tycho from Radio to γ-ray. The γ-ray is mainly accelerated from hadronic processes. BACKGROUND

  4. π0-decay Inverse compton (IC) Nonthermalbremsstrahlung The origin of γ-ray

  5. Thermal emission from material compressed by the FS provides particularly important on particle acceleration in SNRs. The temperature is reduced in the case of efficient acceleration. The fitting result can show the compression ratio. For example, RX J1713.7-3946 eliminates π0- decay for the reason of lack of thermal X-ray emission. Thermal emission of CTB 109 is sufficiently high for π0-decay. Important Thermal emission

  6. C-O Type Ia supernova (spectrum analysis) Distance is uncertain (2-5kpc,4kpc,2.5-3kpc): ejecta velocity; light echo; kinematic methods X-ray emission (ejecta+synchrontron) Ambient density (0.85-2.1 cm^-3, 0.3 cm^-3): X-ray thermal emission; gamma ray flux; expansion index parameters of tycho

  7. CR : cosmic ray HYDRO : hydrodynamics NEI : non-equilibrium ionization Character: 1. non-linear diffusive shock acceleration (DSA) 2. proton and electron spectra coupled with amplified magnetic field. The Cr-hydro-nei model

  8. Lee et al. 2012

  9. Good: evolving full particle spectrum Spatially-resolved A self consistent model Assumption: Spherically symmetric Star with a ejecta density distribution (1.4 Msun) good and assumption

  10. Initial parameters: d, n0, B0, E51, DSA efficiency modeling

  11. testing

  12. sed

  13. Synchrotron IC Nonthermalbremsstrahlung * including the secondary electrons Π0-decay (Kamae et al. 2006) Calculation of model

  14. Model b lower density

  15. IC dominate

  16. NE nonthermal + thermal ?

  17. NW & W

  18. X-ray shock fit well, but declines more slowly than observed brightness behind the shock. Radio fit well with a slow rise to a plateau-like region behind the shock, but not well. because the radio emitting electrons do not suffer significant radiative losses. (R-T increase B) X-ray and radio

  19. Model c

  20. Model c (high density)

  21. n0 : 0.4 cm ^-3 the density out the cavity is low the ionization can be higher due to wind region Include the 0.4 pc wind shell in the model Stellar wind : 3*10^-6 Msun/year V_wind=10 km/s Result is similar to Model A (n0, profile) Because the mass is low (0.1 to 2.5) wind cavity model

  22. Prefer Model A Exist of R-T 1. cause the CD larger than the model 2. the spectra fitting discussion

  23. Ne(0.92), Si (1.85), s(2.45)

  24. 1.Fit with single self-consistent model constrain the density and distinction of pion-decay or IC; without need to add additional component. 2.Fit with continue zones.(DSA) and Consider the MFA 3.include non-adiabatic (turbulence, Alfven wave speed) 4.do not include steep spectrum of protons (p_max=50TeV) Difference with previous

  25. 1. π0-decay in FS is the nature of the γ-ray. IC significant in GeV. 2. Ne/Np=0.003 3. 16% kinetic energy converted to particles 4. proton max energy of 50 TeV 5. distance is 3.2 kpc result

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