Basic seminar II A · Basic seminar II A -+Reviews of Chap. 2-5+-SOKENDAI, M1 Hideaki Takemura...

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Basic seminar II A -+Reviews of Chap. 2-5+- SOKENDAI, M1 Hideaki Takemura 2018/10/05 The physics of fluids and plasmas -An introduction for astrophysicists-

Transcript of Basic seminar II A · Basic seminar II A -+Reviews of Chap. 2-5+-SOKENDAI, M1 Hideaki Takemura...

Page 1: Basic seminar II A · Basic seminar II A -+Reviews of Chap. 2-5+-SOKENDAI, M1 Hideaki Takemura 2018/10/05 The physics of fluids and plasmas -An introduction for astrophysicists-

Basic seminar II A -+Reviews of Chap. 2-5+-

SOKENDAI, M1 Hideaki Takemura

2018/10/05

The physics of fluids and plasmas -An introduction for astrophysicists-

Page 2: Basic seminar II A · Basic seminar II A -+Reviews of Chap. 2-5+-SOKENDAI, M1 Hideaki Takemura 2018/10/05 The physics of fluids and plasmas -An introduction for astrophysicists-

The full set of hydrodynamic equation for neutral fluids- The continuity equation (conservation of mass)

- Incompressible Navier-Stokes equation (conservation of momentum)

- Conservation of energy

∂ρ∂t

+ ∇ ⋅ (ρv) = 0

∂v∂t

+ (v ⋅ ∇)v = −1ρ

∇p + F + ν∇2v

ρ( ∂ϵ∂t

+ v ⋅ ∇ϵ) − ∇ ⋅ (K∇T) + p∇v = 0

Page 3: Basic seminar II A · Basic seminar II A -+Reviews of Chap. 2-5+-SOKENDAI, M1 Hideaki Takemura 2018/10/05 The physics of fluids and plasmas -An introduction for astrophysicists-

The continuity equation (conservation of mass)∂ρ∂t

+ ∇ ⋅ (ρv) = 0

vn

SdS

V

total mass

increase of mass per unit time

the mass flows out from the region V

conservation of the mass

So that this makes ends meet for any arbitrary regions V

∫ ∫ ∫VρdV

∂∂t ∫ ∫ ∫V

ρdV = ∫ ∫ ∫V

∂ρ∂t

dV

∫ ∫Sρv ⋅ n dS = ∫ ∫ ∫V

∇ ⋅ (ρv) dV

∫ ∫ ∫V

∂ρ∂t

dV = − ∫ ∫ ∫V∇ ⋅ (ρv) dV

∫ ∫ ∫V (∂ρ∂t

+ ∇ ⋅ (ρv)) dV = 0

∂ρ∂t

+ ∇ ⋅ (ρv) = 0

Page 4: Basic seminar II A · Basic seminar II A -+Reviews of Chap. 2-5+-SOKENDAI, M1 Hideaki Takemura 2018/10/05 The physics of fluids and plasmas -An introduction for astrophysicists-

The full set of hydrodynamic equation for neutral fluids- The continuity equation (conservation of mass)

- Incompressible Navier-Stokes equation (conservation of momentum)

- Conservation of energy

∂ρ∂t

+ ∇ ⋅ (ρv) = 0

∂v∂t

+ (v ⋅ ∇)v = −1ρ

∇p + F + ν∇2v

ρ( ∂ϵ∂t

+ v ⋅ ∇ϵ) − ∇ ⋅ (K∇T) + p∇v = 0

Page 5: Basic seminar II A · Basic seminar II A -+Reviews of Chap. 2-5+-SOKENDAI, M1 Hideaki Takemura 2018/10/05 The physics of fluids and plasmas -An introduction for astrophysicists-

Incompressible Navier-Stokes equation (conservation of momentum)

∂v∂t

+ (v ⋅ ∇)v = −1ρ

∇p + F + ν∇2v

∇ ⋅ v = 0∂ρ∂t

+ ∇ ⋅ (ρv) = 0The continuity equation

∂ρ∂t

= 0 , ρ = const .

variation

convection

diffusion

internal source external source

dvdt

=Fm

(force per unit mass)

equation of motion

ν =μρ

kinematic viscosity : : viscosity coefficient

Page 6: Basic seminar II A · Basic seminar II A -+Reviews of Chap. 2-5+-SOKENDAI, M1 Hideaki Takemura 2018/10/05 The physics of fluids and plasmas -An introduction for astrophysicists-

The full set of hydrodynamic equation for neutral fluids- The continuity equation (conservation of mass)

- Incompressible Navier-Stokes equation (conservation of momentum)

- Conservation of energy

∂ρ∂t

+ ∇ ⋅ (ρv) = 0

∂v∂t

+ (v ⋅ ∇)v = −1ρ

∇p + F + ν∇2v

ρ( ∂ϵ∂t

+ v ⋅ ∇ϵ) − ∇ ⋅ (K∇T) + p∇v = 0

Page 7: Basic seminar II A · Basic seminar II A -+Reviews of Chap. 2-5+-SOKENDAI, M1 Hideaki Takemura 2018/10/05 The physics of fluids and plasmas -An introduction for astrophysicists-

conservation of energy

ρ( ∂ϵ∂t

+ v ⋅ ∇ϵ) − ∇ ⋅ (K∇T) + p∇v = 0

going in and out of energy with fluids

going in and out of energy due to the heat flow

going in and out of energy due to the work

Page 8: Basic seminar II A · Basic seminar II A -+Reviews of Chap. 2-5+-SOKENDAI, M1 Hideaki Takemura 2018/10/05 The physics of fluids and plasmas -An introduction for astrophysicists-

The full set of hydrodynamic equation for neutral fluids- The continuity equation (conservation of mass)

- Incompressible Navier-Stokes equation (conservation of momentum)

- Conservation of energy

∂ρ∂t

+ ∇ ⋅ (ρv) = 0

∂v∂t

+ (v ⋅ ∇)v = −1ρ

∇p + F + ν∇2v

ρ( ∂ϵ∂t

+ v ⋅ ∇ϵ) − ∇ ⋅ (K∇T) + p∇v = 0

Page 9: Basic seminar II A · Basic seminar II A -+Reviews of Chap. 2-5+-SOKENDAI, M1 Hideaki Takemura 2018/10/05 The physics of fluids and plasmas -An introduction for astrophysicists-

Assumptions

∂ρ∂t

+ ∇ ⋅ (ρv) = 0

∂v∂t

+ (v ⋅ ∇)v = −1ρ

∇p + F + ν∇2v

ρ( ∂ϵ∂t

+ v ⋅ ∇ϵ) − ∇ ⋅ (K∇T) + p∇v = 0

- The continuity equation

- Incompressible Navier-Stokes equation

- Conservation of energy

1. Spatial variation of viscosity μ is neglected.

2. Heat production due to the viscous damping of motion is neglected.

3. Neutral incompressible fluids ∇ ⋅ v = 0

No radiation No chemical evolution

We will consider the solutions of the equations under different circumstance.

Page 10: Basic seminar II A · Basic seminar II A -+Reviews of Chap. 2-5+-SOKENDAI, M1 Hideaki Takemura 2018/10/05 The physics of fluids and plasmas -An introduction for astrophysicists-

Ideal fluids

Viscous flows

Chapter 4, no viscosity

Chapter 5

Page 11: Basic seminar II A · Basic seminar II A -+Reviews of Chap. 2-5+-SOKENDAI, M1 Hideaki Takemura 2018/10/05 The physics of fluids and plasmas -An introduction for astrophysicists-

Euler equation

If ν = 0 (μ = 0),

∂v∂t

+ (v ⋅ ∇)v = −1ρ

∇p + F + ν∇2vIncompressible Navier-Stokes equation

∂v∂t

+ (v ⋅ ∇)v = −1ρ

∇p + F Euler equation

&(v ⋅ ∇) v =

12

∇(v ⋅ v) − v × (∇ × v)

∂v∂t

+ (v ⋅ ∇) v +12

∇(v ⋅ v) − v × (∇ × v) = −1ρ

∇p + F

・F is conservative force ・vorticity ・incompressible fluids

ω = ∇ × vtake a curl

ρ = const .∂ω∂t

= ∇ × (v × ω)

∇ ⋅ v = 0

the complete dynamical theory of incompressible fluids

no viscosity

Page 12: Basic seminar II A · Basic seminar II A -+Reviews of Chap. 2-5+-SOKENDAI, M1 Hideaki Takemura 2018/10/05 The physics of fluids and plasmas -An introduction for astrophysicists-

Newtonian fluidShear force is proportional to the gradient of velocity

Force { acts in a vertical direction on the surface of fluids

acts in a horizontal direction on the surface of fluids pressure

shear force

Tensor Pij = p δij + πij

πij = a ( ∂vi

∂xj+

∂vj

∂xi ) + b δij∇ ⋅ v

The equation of motion &

∂v∂t

+ (v ⋅ ∇)v = −1ρ

∇p + F + ν∇2v Navier-Stokes equation

take a curl ∂ω∂t

= ∇ × (v × ω) + ν∇2ω

ρdvi

dt= ρFi −

∂Pij

∂xj

Page 13: Basic seminar II A · Basic seminar II A -+Reviews of Chap. 2-5+-SOKENDAI, M1 Hideaki Takemura 2018/10/05 The physics of fluids and plasmas -An introduction for astrophysicists-

Reynolds numberFluid flows around geometrically similar object of different sizes

let L, V are the typical length of the object and fluid velocity

x = x′�L, v = v′�V, t = t′�LV

, ω = ω′�VL

x’, v’, t’ and ω’ are the values of length, velocity, time and vorticity measured in these scaled units

∂ω∂t

= ∇ × (v × ω) + ν∇2ω∂ω′�∂t′�

= ∇ × (v′� × ω′�) +1ℛ

∇′�2ω′�

ℛ =LVν

Reynolds numberthe equation is in the scaled variables