WanKee Cho 1 , and Jongsoo Kim 2 Bon-Chul Koo 1

1. Numerical Simulations on the Dynamical Evolution of Supernova Remnants near the Edge of Molecular Clouds WanKee Cho1, and Jongsoo Kim2 Bon-Chul Koo1 1Astronomy Division Department of Physics and Astronomy, Seoul National University 2Korea Astronomy and Space Science Institute

2. Schematic View Explosion depths (2 pc ~ 3.5 pc)tcool = 2500 yearsDcool = 2.75 pc (where, nH = 100 /cm3 ) Density contrasts(100, 1000, 10000)

3. Methods 2. Cooling 1. Code The Cooing function covers wide range of temperature between 10K to 108K, which is modified by various cooling functions. And the heating is considered at the equilibrium temperature and the density. CH = ( Λ – Γ )= nH2 L(T) – nH G(T) = nH(nH L(T) – neqL(Teq)) 3-D rectangular coordinate, parallel with MPI, hydrodynamic TVD code with HLL scheme 3. Calculator KASI – ARCSEC Linux Cluster [Fig.5 The Schematic diagram of the four regions divided by the coloring method]

4. Results z = -2.0 pc : ρ P T vel. t = t0 t = 1,500 yrs t = 12,500 yrs

5. Results Explosion Depths Rs ~ (Sedov stage) t2/5 (after tsf) t3/10-----------------------(toward ICM)D2.0, D2.5 : t3/4D2.75, D3.0, D3.5 t3/5 Density Contrasts Rs ~ (Sedov stage) t2/5 (after tsf) t3/10-----------------------(toward ICM)1000, 10000 : t3/4100 : t3/5

6. High-Resolution study Multiple Shells Clumps& Columns

7. THANK YOU~ ^^*

8. tcool Initial Conditions • Explosion depths (2.0 ~ 3.5)tcool = 2500 yearsDcool = 2.75 pc (where, nH = 100 /cm3 ) (2) Density contrasts(100, 1000, 10000)

9. Discussion (1) High-Resolution study 1/32 pc/grid, when z = -2.5 pc t = 2,500 years Accelerated Region

10. Discussion (1) High-Resolution study 1/32 pc/grid, when z = -2.5 pc t = 3,500 years Accelerated & Diffused Region

11. Results (1) (2) (3) (4) t = t0 t = 1,500 yrs t = 12,500 yrs

12. Results Rs ~ (Sedov stage) t2/5 (after tsf) t3/10(toward ICM) t3/4

13. Coloring

14. Abstract We have carried out 3-D numerical simulations on the dynamical evolution of supernova remnants near the edges of large dense clouds to understand the break-out morphology SNRs. We vary the depth of SN explosion within the cloud and also the density contrast between the cloud and the intercloud medium which are in the pressure equilibrium. We find a power-law relationship between the SNR radius and the age. The closer to the edge of the cloud the SN explodes and the bigger the density contrast is, the exponent converges to 3/4 toward the intercloud medium and to 3/5 in the opposite limit. We carry out a higher (10243) resolution simulation for the case when the SN explodes at 2.5 pc from the cloud edge. We find a clumpy structure in the shell and colliminated gas flow toward the intercloud medium. We explore the origin of these structures.

15. Results (4) Density Contrasts Rs ~ (Sedov stage) t2/5 (after tsf) t3/10-----------------------(toward ICM)1000, 10000 : t3/4100 : t3/5

16. Cooling

17. Contents • Previous works and Modeling • Methods and the Initial conditions_HLL tvd code, cooling function, coloring_initial conditions • Results_z = -2.0 pc and -3.0 pc_radius and age relations • Discussion and Summary_higher resolution simulation; clumpy structure and the collimated gas flow.

18. Previous Works (1) Falle & Galick, 1982 “to explain the velocity field and the emission observed in the various components of the Cygnus Loop”- 2D calculations & only for the adiabatic cases (2) Tenorio-Tagle et al., 1985, (Z-5 case) “(To) describe the evolution of a remnant resulting from supernova explosions…near the molecular clouds” - 2D calculations & adoption of the poor cooling effect (3) Arthur & Falle, 1991 “astrophysical problem of supernova explosions in strong density gradients”

19. Initial Conditions

20. Results (2) z = -3.5 pc : ρ P T vel. t = t0 t = 10,000 yrs t = 30,000 yrs

21. Results (3) (4)

22. Results Rs ~ (Sedov stage) t2/5 (after tsf) t3/10(toward ICM) t3/5