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Toward high-resolved hydrodynamic Simulations of Supernova remnants such as Cas A, Tycho ..

TV meeting 2009.07.24. Toward high-resolved hydrodynamic Simulations of Supernova remnants such as Cas A, Tycho. Masaomi Ono Kyushu University. Contents. Introduction Antecedent studies Calculation toward Tycho SNR Initial condition Method Results Future prospects. Introduction.

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Toward high-resolved hydrodynamic Simulations of Supernova remnants such as Cas A, Tycho ..

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  1. TV meeting 2009.07.24 Toward high-resolved hydrodynamic Simulations of Supernova remnantssuch as Cas A, Tycho .. Masaomi Ono Kyushu University

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

  3. Introduction

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

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

  6. SNR observations 3 (Tycho) • Ion X-ray emmitions • Ion temperature(1-3)×1010 K Furuzawa et al. 2009

  7. Antecedent studies

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

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

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

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

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

  13. Calculation toward Tycho SNR

  14. Initial condition • Carbon deflagration model (W7) • Nomoto, Thielemann & Yokoi 1984 • Density, temperature, chemical compositionradial velocity • Ambient medium • ρAM = ～10-25 gcm-3 (1 個 cm-3) • T = 103 K

  15. Initial chemical composition 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= ∫κρdr = 2/3 (κ: electron scattering) • α-network (Müller 1986) • 4He, 12C, 16O, 20Ne, 24Mg, 28Si, 32S, 36Ar, 40Ca, 44Ti, 48Cr, 52Fe, 56Ni

  17. Density

  18. Energy density

  19. Temperature

  20. Density profile

  21. Radial velocity profile

  22. Mass fraction

  23. Problems • Oscillation • Rezoning & mapping ?

  24. Future prospects

  25. High-resolution MHD simulation • AMR (Adaptive Mesh Refinement) • Berger & Oliger 1984; Berger & Colella 1989 AMR (3D) ＋ Nucleosynthesis ＋ Magnetic field 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) ZEUS-MP + AMR + Network v.s. FLASH ?

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

  28. Synthetic radio emission Orlando et al. 2007

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