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Marco Miceli , INAF – Osservatorio Astronomico di Palermo Consorzio COMETA, Italy

5 th Jetset School on High Performance Computing in Astrophysics 8 th -13 th January 2008 Galway, Ireland. Hydrodynamic evolution of ejecta in the Vela SNR. Marco Miceli , INAF – Osservatorio Astronomico di Palermo Consorzio COMETA, Italy. Collaborators

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Marco Miceli , INAF – Osservatorio Astronomico di Palermo Consorzio COMETA, Italy

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  1. 5th Jetset School on High Performance Computing in Astrophysics 8th-13th January 2008 Galway, Ireland Hydrodynamic evolution of ejecta in the Vela SNR Marco Miceli, INAF – Osservatorio Astronomico di Palermo Consorzio COMETA, Italy Collaborators F. Bocchino, INAF – Osservatorio Astronomico di Palermo, Italy F. Reale, INAF – OAPa, Università di Palermo, Italy S. Orlando, INAF – Osservatorio Astronomico di Palermo, Italy

  2. Supernova Remnants • Supernova explosion • Total energy released:  1053erg • “Visible” energy:  1051erg • Mass ejected: several solar masses G292.0+1.8 • Heating of the ambient medium • Compression • Interaction with interstellar clouds • Formation of blast wave shocks • Chemical enrichment of the galaxy • Propagation of supersonic “bullets” • Propagation of the ejecta

  3. The Vela SNR The Vela SNR Distance: ~250 pc Age: ~11000 yr In middle-aged SNR the bulk of the X-ray emission is commonly associated with shocked ISM, but: Vela SNR:6 X-ray emitting “shrapnels”, that are probably associated with ejecta (outside the border of the shell). Recent discovery of new shrapnels inside the shell (Miceli et al. 2007, ApJ accepted) 0.1-2.3 keV Rosat All Sky Survey

  4. Hydrodynamic modeling Aims:evolution of supersonic fragments of ejecta (interaction with the shock waves and with the ambient medium) Equations of the model: r: mass density v: bulk velocity P: pressure E: tot. energy per unit mass q: -k(T)T (Spitzer & saturated) n: density L(T): radiative losses function e: internal energy per unit mass P= Numerical solution through the FLASH HD code (Fryxell, 2000)

  5. Hydrodynamic modeling • Initial conditions:exploding sphere • of ejecta with a density inhomogeneity • (i. e. the shrapnel) • Mej = 12 M⊙ • E = 1051 erg • R0 = 4.5 x 1018 cm • Vej(R0) = 6 x 1018 cm/s (v(R)  r) • r (R) following Wang & Chevalier 2002 • Mshrapnel = 1/20 Mej • rshrapnel = crej • 2-D simulations in cylindrical coordinates (axial symmetry). We follow the evolution of the system for ~ 15000 yr (the Vela age is ~ 11000 yr) z (cm) r (cm)

  6. Hydrodynamic modeling Parameter space exploration(*):We investigate how the evolution of the system depends on the density contrast (between the shrapnel and the surrounding ejecta) and on the initial position of the shrapnel. Pure HD run (no thermal cond. no rad. losses) executed on the HPC system COMETA (total CPU time~250 h, memory~7 Mb, output size~3 Gb). Rshrapnel/R0 “Complete” run executed on the CINECA CLX cluster (total CPU time~9000 h) c “Complete” runs to be done on the COMETA HPC system (*) Work in progress…

  7. Hydrodynamic modeling The Vela SNR 0.1-2.4 keV ROSAT All SKy Survey (0.1-2.4 keV) The “pure HD” run: (c = 30, Rshr = 1/3 R0) spatial res. 2048 x 2048 point logr (g/cm3) T (K)

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