1. New evidence for strong nonthermal effects in Tycho’s supernova remnant Leonid Ksenofontov 1 H.J.Völk 2, E.G.Berezhko 1, 1 Yu.G.Shafer Institute of Cosmophysical Research and Aeronomy, Yakutsk, Russia 2 Max-Planck-Institut f ü r Kernphysik, Heidelberg, Germany ksenofon@ikfia.ysn.ru The Multi-Messenger Approach to High Energy Gamma-ray Sources, Barcelona, July 4-7, 2006

2. The model: supernova explosion VpVp VsVs shock wave ejecta (piston) supernova CRs ISM: n H (~1 – 100 cm -3 ) T (~10 4 – 10 6 K) B 0 (~1 – 100 μG) SN: E SN (~10 51 erg) M ej (~1 M sun ) V p0 (~10 5 km/s) diffusive shock acceleration

3. The model: basic equations Hydrodynamic equations CR transport equations for protons and electrons CR pressure Injection term ρ(r, t) – gas density w(r, t) – gas velocity P g (r, t) – gas pressure f(p, r, t) – CR distribution function CR diffusion coefficient Synchrotron loss time

4. Völk et al. 2002, 2005 About 10% of the explosion energy has been transferred into CR energy up to now, which means that the CR energy content is E c = 0.1 E sn.

5. Distance determinations to Tycho’s supernova:  From the optical measurements d = 2.3 ± 0.8 kpc (Smith et al. 1991)  It is hard to escape from the uncertain range 2 – 4 kpc with the analyses done so far (Ruiz-Lapuente 2004) What’s new:  From the Chandra measurements Warren et al. (2005) estimate a mean ratio of contact discontinuity (ejecta) radius to blast wave radius as 0.93  Badenes et al. (2005) found that the properties of the X-ray emission are well reproduced by a 1D delayed detonation model with a kinetic energy of ~ 1.2 × 10 51 erg.

6. Qualitative estimate of gamma-ray flux In the Sedov phase - constant

8. 3D Simulations by Blondin & Ellison (2001) Correction factor 1.05

10. The ratio of the radii of the contact discontinuity and the forward shock

11. Spectral energy distribution of the gamma-rays

12. Conclusions:  HEGRA Upper Limit is consistent with the distance 3.3 − 4 kpc  The expected π 0 -decay γ-ray energy flux is (2 − 5)×10 −13 erg/(cm 2 s)  The new Northern hemisphere IACT such as MAGIC, VERITAS will be able to detect Tycho’s SNR  TeV gamma-rays predominantly have hadronic origin  Detection of a TeV signal is also important for the correct determination of key Supernova parameters

13. Kepler’s SNR

14. Total (π 0 -decay + IC) integral γ-ray energy fluxes as a function of γ-ray energy for the same four cases as in Fig.1. For comparison, the respective sensitivities for a 5σ detection in one year with GLAST (Weekes 2003, Proc. 28th ICRC, 8, 3), and in 50 hours at 20º zenith angle for a photon index 2.6 (as for the Crab Nebula) with H.E.S.S. (Funk 2005, in PhD thesis), are shown.