Series Lecture on Laser Plasma Physics

Professor, Institute of Laser Engineering andSchool for Physics and School for Space and Earth Science,

Graduate School of Science, Osaka University, Japan

Visiting Professor, Shanghai Jiao Tong UniversityShanghai, China

 H. Takabe (Aki)

at Shanghai Jiao Tong UniversityJune 27&28, July 4&5, 2009

1

Chapter 1

Introduction

2

1.1 Self-introduction

3

4

Creation of Mimic Black Hole in LaboratoryILE OSAKA

Takabe-G: Laser Astrophysics (1)

Black Hole Experimental Data　　　

Black Hole

Neutron Star　　

Photo-ionization in X-ray Binary with Black Hole

Universe

Laboratory

Radiation Temperature of 0.5 keV has been achieved.

5

Challenging 100 year-standing mystery of Cosmic Ray 　　　　　　　　 = Collisionless Shock Physics = ILE OSAKA

Averaged Density

Self-Generated E and B fields

Space

Shock Jump

30 Li

ght

Year

s

Shock Front

Collisionless Shock Formation by Self-Organization (Kato-Takabe Theory)

Density

Universe

Laboratory

SN1006

Takabe-G: Laser Astrophysics (2)

6

1.2 High-Power Laser

Maiman (1960)

Ruby Laser

7

Early Stage of Laser for Inertial Confinement Fusion in Livermore, USA

8

What is laser?

9

Laser Welding

10

Gekko XII Laser, Osaka Univ.

ILE, Osaka University

Gekko Amplifiers

Big Laser Facilities

Nonlinear Optics

Harmonic Conversion with Nonlinear Crystal

Shorter Wavelength is better for Laser Plasma Interaction

11

12

What is Plasma ?1.3 Plasmas

Solid Liquid Gas

Plasmas

13

14

15

1.4 Plasmas in Nature and LifeLightening

16

17

How gamma-ray appears accompanied with lightening

18

19

Solar Flare

20

21

Plasmas

22

Corona Mass Ejection

23

Aurora

24

Plasmas

藤井旭、「星のたんじょう」（金の星社）

1.5 Plasmas in Universe

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26

27

28

Planetary Nebula(Hour Glass Nebula)

Hubble Space Telescope(NASA)

29

30

Supernova Explosion

31

Crab Nebula and Neutron Star

Quark Gluon PlasmaBefore collision After collision

中性子星

ビッ

グバ

ン

32

Structure of SunSurface ： 6000K

Center:1.5keV 33

Convection near the surface of the Sun

34

35

Temperature Density

36

37

38

Lorentz force and gyro motion

)( Bvvq

dtdm

Bvqvmc

2

mBqv

Bqmv

ccc

1.6 How to describe Plasmas

39

Drift motion

)( BvEvq

dtdm

BB'BvEE' E

)'''(' BvEv

qdtdm

2EE B0 BEvBvEE'

40

Maxwell Equations

E Bt

10

B j 0Et

0E

B 0

Faraday’s Law

Ampere’s Law

Poisson Equation

Absence of Magnetic Monopole

41

42

Hydrodynamic Equationsnt

(nu) 0

mt

u

u 1nP q E u B

mdudt

1nP q E u B

ddt

PdVdt

dQdt

Continuity

Motion

Energy

0)n(t

nii

i u

BuEuu

iiii

iii e)Tn(n1

tm

0)n(t

nee

e

u

BuEuu

eeee

eee e)Tn(n1

tm

ei en-en=

eeii en-en= uuj

t

BE

t1

00

EjB

E0

0 B

Ion Fluid

Electron FluidMaxwell Equations

Charge and Current Densities

Basic Equations for Plasma Fluid Model

43

44

Ludwig Boltzmann (1844-1906)Suicide in 1906

S = -k ln W

Boltzmann wrote in1898 “I am conscious of being only an individual struggling weakly against the stream of time.” Increasingly subject to depressions, Boltzmann committed suicide in 1906 only shortly before Perrin’s experiment on Brownian motion (1908) and Mililan’s oil-drop experiment (1909) provided very direct evidence for the discrete structure of matter.

(Statistical Physics, Berkeley Phys. 5)P. 162

45

Boltzmann Equationdfdt

ft

drdt

fr

dvdt

fv

dfdt

coll

drdt

vdvdt

Fm

ft

vfr

Fm

fv

dfdt

coll

f(t,r,v): Velocity distribution function

Vlasov Equation

46

From Particle Image to Fluid Image

(Particles) (Ensembles)

(Phase Space)

(Distribution Func.)(Real Space)

(Moment Eqs.)

[CE expansion]

[Velocity moments]

(Fluid Eqs.)

[E.A.]

47

Fokker-Planck Equation

48

),,(),(),(),,(),,(1WWWW

rtrtrtrtrttc

III

III

xtc1

IIII

rrtc)1(1 2

Radiation Transport Equation

49

Hamiltonian for N-electron system

How to solve:MCHF, HF, Para-potential MethodOPAL at LLNL 50

Rate Equations

51

Appendix A

Historical Events of

Plasma Physics

52

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Appendix B

54

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56

57

58

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60

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