1. image: http://chandra.harvard.edu/photo/2006/casa/ Toward high-resolved hydrodynamic Simulations of Supernova remnants such as Cas A, Tycho.. Masaomi Ono Kyushu University TV meeting 2009.07.24 1

2. Contents Introduction Antecedent studies Calculation toward Tycho SNR – Initial condition – Method – Results Future prospects 2

3. Introduction 3

4. SNR observations 1 (Tycho) X-ray image – Red: Fe L-shell – Green: Si K-shell – Blue: high energy 1 : 0.93 : 0.70 (BW:CD:RS) 4 Warren et al. 2005 Chandra X-ray image

5. Spectrum – Featureless – Ejecta 5 Warren et al. 2005 SNR observations 3 (Tycho)

6. Ion X-ray emmitions Ion temperature (1-3)×10 10 K 6 Furuzawa et al. 2009 SNR observations 3 (Tycho)

7. Antecedent studies 7

8. Thermal X-ray emission from shocked ejecta in Type Ia SNR 1 Explosion mechanisms – DET – SCH – DEF – DDT – PDD 8 Badenes et al. 2003; Badenes et al. 2005

9. Plasma model & Ionization calculation 9 Badenes et al. 2003; Badenes et al. 2005

10. Calculated synthetic spectrum Hamilton & Sarazin code + XSPEC software package 10 Badenes et al. 2003; Badenes et al. 2005

11. 11 Wheeler, Maund & Couch 2008 Proposed jet direction Proper motion of compact object Holes The shape of Cas A 1

12. The shape of Cas A 2 High-resolution hydrodynamic simulation – FLASH Code (Fryxell et al. 2000) 12 Wheeler, Maund & Couch 2008 Jet

13. 13 Calculation toward Tycho SNR

14. Initial condition Carbon deflagration model (W7) – Nomoto, Thielemann & Yokoi 1984 Density, temperature, chemical composition radial velocity Ambient medium – ρ AM = ～ 10 -25 g cm -3 (1 個 cm -3 ) – T = 10 3 K 14

15. Initial chemical composition 15 Thielemann, Nomoto & Yokoi 1986

16. Method & input physics Hydrodynamic simulation – Cede: ZEUS-2D – EoS Ideal gas + radiation (optically thick) P = K ργ, e = P / (γ - 1) (optically thin) τ = ∫ κ ρ dr = 2/3 (κ: electron scattering) – α-network (Müller 1986) 4 He, 12 C, 16 O, 20 Ne, 24 Mg, 28 Si, 32 S, 36 Ar, 40 Ca, 44 Ti, 48 Cr, 52 Fe, 56 Ni 16

17. Density 17

18. Energy density 18

19. Temperature 19

20. Density profile 20

21. Radial velocity profile 21

22. Mass fraction 22

23. Problems Oscillation – Rezoning & mapping ? 23

24. 24 Future prospects

25. High-resolution MHD simulation AMR (Adaptive Mesh Refinement) – Berger & Oliger 1984; Berger & Colella 1989 25 Magnetic fieldAMR (3D)Nucleosynthesis ＋＋ How we achieve the aim ?

26. Hydrodynamic Codes FLASH – PARAMESH AMR package – 3D, MPI, small nuclear reaction network – Two MHD units (8wave or USM) – Ionization unit (NEI) ZEUS-MP – 3D, MPI, magnetic field (MOC-CT) radiation HD (FLD) 26 ZEUS-MP + AMR + Network v.s. FLASH ?

27. FLASH with magnetic field On the origin of asymmetries in bilateral supernova remnants – 3D MHD simulations by FLASH code 27 Orlando et al. 2007 Initial distributions of density & magnetic field

28. Synthetic radio emission 28 Orlando et al. 2007