image: http://chandra.harvard.edu/photo/2006/casa/

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

Masaomi OnoKyushu University

TV meeting2009.07.24

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Contents

• Introduction• Antecedent studies• Calculation toward Tycho SNR– Initial condition–Method–Results

• Future prospects

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Introduction

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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)

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Warren et al. 2005

Chandra X-ray image

• Spectrum– Featureless– Ejecta

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Warren et al. 2005

SNR observations 3 (Tycho)

• Ion X-ray emmitions

• Ion temperature(1-3)×1010 K

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Furuzawa et al. 2009

SNR observations 3 (Tycho)

Antecedent studies

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Thermal X-ray emission from shocked ejecta in Type Ia SNR 1

• Explosion mechanisms– DET– SCH– DEF– DDT– PDD

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Badenes et al. 2003; Badenes et al. 2005

Plasma model & Ionization calculation9

Badenes et al. 2003; Badenes et al. 2005

Calculated synthetic spectrum

• Hamilton & Sarazin code + XSPEC software package

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Badenes et al. 2003; Badenes et al. 2005

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Wheeler, Maund & Couch 2008

Proposed jet direction Proper motion of compact object

Holes

The shape of Cas A 1

The shape of Cas A 2

• High-resolution hydrodynamic simulation– FLASH Code (Fryxell et al. 2000)

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Wheeler, Maund & Couch 2008

Jet

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Calculation toward Tycho SNR

Initial condition

• Carbon deflagration model (W7)– Nomoto, Thielemann & Yokoi 1984• Density, temperature, chemical composition

radial velocity

• Ambient medium– ρAM = ～ 10-25 g cm-3 (1 個 cm-3)

– T = 103 K

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Initial chemical composition15

Thielemann, Nomoto & Yokoi 1986

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)• 4He, 12C, 16O, 20Ne, 24Mg, 28Si, 32S, 36Ar, 40Ca,

44Ti, 48Cr, 52Fe, 56Ni

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Density17

Energy density18

Temperature19

Density profile20

Radial velocity profile21

Mass fraction22

Problems

• Oscillation– Rezoning

& mapping ?

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Future prospects

High-resolution MHD simulation

• AMR (Adaptive Mesh Refinement)– Berger & Oliger 1984; Berger & Colella 1989

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Magnetic fieldAMR (3D) Nucleosynthesis＋ ＋

How we achieve the aim ?

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)

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ZEUS-MP + AMR + Network v.s. FLASH ?

FLASH with magnetic field

• On the origin of asymmetries in bilateral supernova remnants– 3D MHD simulations by FLASH code

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Orlando et al. 2007

Initial distributions of density & magnetic field

Synthetic radio emission28

Orlando et al. 2007