multiple spiral branches on late agb stars qian wang iowa state university

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Multiple spiral branches on late AGB stars Qian Wang Iowa State University

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Page 1: Multiple spiral branches on late AGB stars Qian Wang Iowa State University

Multiple spiral branches on late AGB stars

Qian WangIowa State University

Page 2: Multiple spiral branches on late AGB stars Qian Wang Iowa State University

LL pagasi (Sahai 2010)

Sahai 2006

Page 3: Multiple spiral branches on late AGB stars Qian Wang Iowa State University

Model method

Bowen code Passing planet

+

Page 4: Multiple spiral branches on late AGB stars Qian Wang Iowa State University

Bowen code

• 1-D code with Lagrange zoning.• Hydrodynamic and thermodynamic equation

without magnetic field.• Atmosphere is driven by a sinusoidal piston

below photosphere.• Density dependent thermal relaxation and

Hydrogen cooling at high temperature• Radiation on dust grain and molecules

Page 5: Multiple spiral branches on late AGB stars Qian Wang Iowa State University

Companion characters

• The companion is on a circular orbit. • The mass of the companion ~ 10Mjupiter• The size of the companion is determined by

the average Jupiter density.• The companion has no collision cross section

but only gravity.

Page 6: Multiple spiral branches on late AGB stars Qian Wang Iowa State University

Model parametersMass(Msun) 1

Luminosity(Lsun) 5000

T(K) 2966

R(Rsun) 267.8

Vterminal(km/s at 18R*) 9.35km/s

Mdot(Msun/yr) 1.25e-6

Pulsation period (day) 394

Pulsation Amp.(km/s) 3.974km/s

Page 7: Multiple spiral branches on late AGB stars Qian Wang Iowa State University

Model parametersModel NO. Mp(Mjupit

er)D (Rstar) Porb (days) # of spirals Tss (Ppuls)

1 2 1.01889 522.43 4 60

2 5 1.01889 522.43 4 60

3 5 1.1 586.1 3 60

4 8 1.1 586.1 3 60

5 10 1.1 586.1 3 60

6 12 1.1 586.1 3 60

7 10 1.325 775.082 2 60

8 10 1.339 786.94 2 400

9 10 12.94 23640 1 60

10 20 18.187 39400 1 100

Page 8: Multiple spiral branches on late AGB stars Qian Wang Iowa State University

Origin of super shocksSuper shock clustering Shock speed vs Shock Density

Page 9: Multiple spiral branches on late AGB stars Qian Wang Iowa State University

Shock effectsStrong shocks and Temp. contour Weak shocks and Temp. Contour

Page 10: Multiple spiral branches on late AGB stars Qian Wang Iowa State University

Shock effectsStrong shocks and Molecular accel. contour Strong shocks and dust accel. contour

Page 11: Multiple spiral branches on late AGB stars Qian Wang Iowa State University

Model analysisDensity Profile at time = 700 cycles

Extended density contour of Model 5 at time = 1200 cycles

Model 6

Model 5

Model 4

Model 3

Page 12: Multiple spiral branches on late AGB stars Qian Wang Iowa State University

3 spiral armsDensity color map of Model 5 Kinetic Temperature map of Model 5

Page 13: Multiple spiral branches on late AGB stars Qian Wang Iowa State University

R(cm)

Time (cycle)

Density color map

Page 14: Multiple spiral branches on late AGB stars Qian Wang Iowa State University

4 spiral armsDensity color map of Model 1 Density color map of Model 2

Page 15: Multiple spiral branches on late AGB stars Qian Wang Iowa State University

4 spiral armsDensity Profile at time = 700 cycles Model 1 Density Profile at time = 700 cycles Model 2

Page 16: Multiple spiral branches on late AGB stars Qian Wang Iowa State University

2 spiral armsDensity color map of Model 7 Density color map of Model 8

Page 17: Multiple spiral branches on late AGB stars Qian Wang Iowa State University

2 spiral armsDensity Profile at time = 700 cycles Model 7 Density Profile at time = 700 cycles Model 8

Page 18: Multiple spiral branches on late AGB stars Qian Wang Iowa State University

1 spiral armDensity color map of Model 9 Density color map of Model 10

Page 19: Multiple spiral branches on late AGB stars Qian Wang Iowa State University

1 spiral armDensity Profile at time = 700 cycles Model 9 Density Profile at time = 700 cycles Model 10

Page 20: Multiple spiral branches on late AGB stars Qian Wang Iowa State University

Equation for super shocks

Pss =Ppuls × Porb

Porb −N × (Porb − Ppuls)

Page 21: Multiple spiral branches on late AGB stars Qian Wang Iowa State University

Observation results

IRC-10216 (Mauron & Huggins 2000)

Page 22: Multiple spiral branches on late AGB stars Qian Wang Iowa State University

Questions and suggestions

Maybe I can explain this