Numerical Simulations on the Dynamical Evolution
This presentation is the property of its rightful owner.
Sponsored Links
1 / 22

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


  • 66 Views
  • Uploaded on
  • Presentation posted in: General

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

Download Presentation

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

An Image/Link below is provided (as is) to download presentation

Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author.While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server.


- - - - - - - - - - - - - - - - - - - - - - - - - - E N D - - - - - - - - - - - - - - - - - - - - - - - - - -

Presentation Transcript


Wankee cho 1 and jongsoo kim 2 bon chul koo 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


Schematic view

Schematic View

Explosion depths (2 pc ~ 3.5 pc)tcool = 2500 yearsDcool = 2.75 pc (where, nH = 100 /cm3 )

Density contrasts(100, 1000, 10000)


Methods

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]


Results

Results

z = -2.0 pc : ρ P T vel.

t = t0

t = 1,500 yrs

t = 12,500 yrs


Wankee cho 1 and jongsoo kim 2 bon chul koo 1

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


Wankee cho 1 and jongsoo kim 2 bon chul koo 1

High-Resolution study

Multiple Shells

Clumps& Columns


Wankee cho 1 and jongsoo kim 2 bon chul koo 1

THANK YOU~ ^^*


Initial conditions

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)


Discussion

Discussion

(1) High-Resolution study 1/32 pc/grid, when z = -2.5 pc

t = 2,500 years

Accelerated Region


Discussion1

Discussion

(1) High-Resolution study 1/32 pc/grid, when z = -2.5 pc

t = 3,500 years

Accelerated & Diffused Region


Results1

Results

(1) (2) (3) (4)

t = t0

t = 1,500 yrs

t = 12,500 yrs


Results2

Results

Rs ~

(Sedov stage)t2/5 (after tsf) t3/10(toward ICM)t3/4


Coloring

Coloring


Abstract

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.


Wankee cho 1 and jongsoo kim 2 bon chul koo 1

Results

(4) Density Contrasts

Rs ~

(Sedov stage) t2/5 (after tsf) t3/10-----------------------(toward ICM)1000, 10000 : t3/4100 : t3/5


Cooling

Cooling


Contents

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.


Previous works

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”


Initial conditions1

Initial Conditions


Results3

Results

(2) z = -3.5 pc : ρ P T vel.

t = t0

t = 10,000 yrs

t = 30,000 yrs


Wankee cho 1 and jongsoo kim 2 bon chul koo 1

Results

(3) (4)


Results4

Results

Rs ~

(Sedov stage)t2/5 (after tsf) t3/10(toward ICM)t3/5


  • Login