Download Introduction to High Energy Density Physics

Introduction to
High Energy Density Physics
(HEDP)
R. Paul Drake
University of Michigan
Summer School on High Energy Density Physics
UCSD, July 2011
Department of Atmospheric
Oceanic & Space Sciences
Applied Physics Program
DrakeLab
Michigan Institute for Plasma
Science and Engineering
Center for Radiative
Shock Hydrodynamics
This talk will cover
• Connections between HEDP and other physics
• How to create HED conditions
• Fundamental areas of HEDP
– With some examples
• Some applications of HEDP
2011 Summer School
Intro to High Energy Density Physics
Page 2
Precursors to high-energy-density physics
•
First half 20th Century: Stellar structure
– Eddington, Chandrasekhar, Schwarzschild, among others
•
Mid-20th Century: Nuclear weapons
– Oppenheimer, Sakharov, Teller, Bethe, Fermi, others
• Compressible metals!
– Zelʼdovich and Raizer 1966
• Physics of Shock Waves and High Temperature Phenomena
•
Post Mid-20th Century (1960-1980): Inertial fusion origins
– Nuckolls, Basov, Emmett, others
•
I date HEDP as a discipline from about 1979
– Complex quantitative physics experiments became feasible
– The first user facility program (NLUF at Omega) began in 1979
2011 Summer School
Intro to High Energy Density Physics
Image credit NNSA Nevada Site Office
Page 3
We will use this plot to see aspects of highenergy-density physics (HEDP)
•
•
HEDP parameters
Physics connections
– Strong coupling
– Pressure and Fermi
degeneracy
•
•
Astrophysics
connections
Plasma physics
connections
– Particles per Debye
sphere
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Intro to High Energy Density Physics
Page 4
Physics connections within and beyond HEDP
Quark-gluon
plasmas
QM
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Intro to High Energy Density Physics
Page 5
HEDP plasmas can be very strongly coupled
Electron
Temperature
Te (eV)
•
Γ = |qφ|/kT
X-ray Thomson scattering
2011 Summer School
Intro to High Energy Density Physics
Data from Glenzer & Redmer, RMP 2008
Page 6
Astrophysics connections with HEDP
•
Other elements of this
connection
– High Mach number
flows
– Fast shocks
– Ionizing
– Strong B fields
– Radiation matters
– Plasma
hydrodynamics
2011 Summer School
Intro to High Energy Density Physics
Curves credit NRC report on HEDP
Page 7
Perspectives on plasma physics and HEDP
•
The mid-20th-Century approach to plasma physics, as seen
in most textbooks, was simple
– Many particles per Debye sphere often as the definition of
“plasma”
– Quasineutral
– Only hydrogen
– Spatially uniform
– Maxwellian distributions
– Deviations from spatial uniformity or Maxwellians drive
instabilities
•
21st Century plasma physics breaks these and other
assumptions
– An era of creation and control of systems that deviate strongly
from the simple cases
– High-energy-density plasmas are very much a case in point
2011 Summer School
Intro to High Energy Density Physics
Page 8
HEDP systems often have
few particles per Debye sphere
Be model
UV Thomson scattering
2011 Summer School
Image credit David Montgomery
Intro to High Energy Density Physics
Data credit Riccardo Betti
Page 9
Regime boundaries move as materials change
Ionization is
centrally important
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Intro to High Energy Density Physics
Page 10
The pressure often is not nkT
~ Gbar shock
in Al
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Intro to High Energy Density Physics
Page 11
Data from Cauble et al, PRL 1991
HEDP theory: a fluid approach often works, but
not always
•
Most phenomena can be grasped using a single fluid
– with radiation,
– perhaps multiple temperatures,
– perhaps heat transport, viscosity, other forces
•
A multiple fluid (electron, ion, perhaps radiation or other ion)
approach is needed at “low” density
•
Magnetic fields sometimes matter
•
Working with particle distributions (Boltzmann equation and
variants) is important when strong waves are present at “low”
density
•
A single particle or a PIC (particle-in-cell) approach is needed for
the relativistic regime and may help when there are strong waves
2011 Summer School
Intro to High Energy Density Physics
Page 12
We now discuss
how to create HEDP conditions
2011 Summer School
Intro to High Energy Density Physics
Page 13
So how does one start HEDP dynamics?
•
Shoot it, cook it, or zap it
•
Shoot a target with a “bullet”
– Pressure from stagnation against a very dense bullet ~ ρtarget (vbullet)2/2
– 20 km/s (2 x 106 cm/s) bullet at 2 g/cc gives ~ 4 Mbar
•
Cook it with thermal x-rays
– Irradiance σT4 = 1013 (T/100 eV)4 W/cm2 is balanced by outflow of
solid-density matter at temperature T and at the sound speed
so
T / Mi
!T 4 = " T / M i = p T / M i /(# $1)
– From which
2011 Summer School
p = (! "1) M i #T 3.5
$ T '
~ 20&
)
%100 eV (
Intro to High Energy Density Physics
3.5
Mbars
Page 14
… or zap it with a laser
Laser beam
Any material
Thicker layer for
Laser: 1 ns pulse (easy)
diagnostic
≥ 1 Joule (easy)
Irradiance ≥ 1013 W/cm2
(implies spot size of 100 µm at 1 J,
1 cm at 10 kJ)
Emission
From rear
Time
This produces a pressure ≥ 1 Mbar (1012 dynes/cm2, 0.1 TP).
Momentum balance gives p ~ 3.5 I142/3 / λµm2/3 Mbars
This easily launches a shock.
Sustaining the shock takes more laser energy.
2011 Summer School
Intro to High Energy Density Physics
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Perspectives on strong shocks in HEDP
• Many HEDP experiments involve at least one
strong shock
– A natural consequence of depositing kJ/mm3 in matter
• Strong shocks are useful!
– In Inertial Confinement Fusion
– For equation of state measurements
– As sources of energy or momentum
Shock in Xe clusters
• Radiative shocks
• Isentropic compression
• Hydrodynamic processes
2011 Summer School
Intro to High Energy Density Physics
Page 16
Data from Ditmire et al. ApSS 2000
High Energy Lasers are key tools
• High energy lasers amplify the light energy
across a large area then compress the beam(s) in
space to create high energy density
vacuum
amplify
protect
irradiate
Smooth
(spatial filter)
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Intro to High Energy Density Physics
amplify
Page 17
The biggest lasers can produce 100 Mbar pressures
on mm2 to cm2 areas
Omega
60 beams
30 kJ
Target chamber at Omega laser
National Ignition
Facility
192 beams
> 1 Megajoule
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Page 18
The laser creates structure at the target surface
•
The laser is absorbed at less than 1% of solid
density
Ablation pressure
from approximate
momentum balance:
p ~ 3.5 I142/3 / λµm2/3 Mbars
This is a bit low; better
calculations replace
3.5 by 8.6
A pressure > 100
Mbars is practical
From Drake, High-Energy-Density Physics, Springer (2006)
2011 Summer School
Intro to High Energy Density Physics
Page 19
Hohlraums create thermal environments at
millions of degrees
•
Put energy inside a
high-Z enclosure
•
The vacuum
radiation field stays
in equilibrium with
the resulting hot
surface
Laser spots seen through thin-walled hohlraum.
Credit LLNL
Hohlraum with experiment attached on bottom
•
One gets high
temperatures
because the radiation
wave moves slowly
into the material,
penetrating few
microns
2011 Summer School
Intro to High Energy Density Physics
From Drake,
High-EnergyDensity
Physics,
Springer (2006)
Page 20
Z pinches also produce high-energy-density
conditions
•
Todayʼs biggest is the Z machine at Sandia, when run as a
Z pinch (~ 2 MJ of x-rays)
•
Z pinches exploit the attraction between parallel currents
Cylindrical wire array
Implosion
Stagnation
Credit:
Keith Matsen
Inward J X B force
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Inward
acceleration
Intro to High Energy Density Physics
Shock heating &
Radiative cooling
Page 21
The action is at the center of a large though
compact structure
2011 Summer School
Intro to High Energy Density Physics
Credit:
Keith Matsen
Page 22
Ultrafast lasers produce
relativistic HED conditions
•
•
Compression in time as well as space
Hercules at U. Michigan
– The most intense laser in the world
ao = p/mc ~ 100
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Particle beam bunches can be HED systems
Located at SLAC
e-
Ionizing
Laser Pulse Li Plasma
(193 nm) ne!6·10 15 cm-3
L!30 cm
Streak Camera
(1ps resolution) "Cdt
N=1-2·1010
!z=0.1 mm
Optical Transition Spectrometer Cerenkov
E=30 GeV
Radiator
Radiators
m
25 m
2011 Summer School
Slide Credit: Chan Joshi
X-Ray
Diagnostic
Dump
Not toIntro
scale!
to High Energy Density Physics
FFTB
Page 24
Now we turn to the fundamental physics of
HEDP systems
•
In a traditional sense HED plasma properties are weird
–
–
–
–
Cannot assume Z = 1
Cannot assume the ion mass is the hydrogen mass
Cannot assume only one ion species
Cannot assume the plasma is always an ideal gas
•
This weirdness affects their Equations of State
•
These plasmas also exhibit a lot of crazy dynamics
–
–
–
–
–
Shock waves and things they make happen
Plasma wakes and things they make happen
Gigagauss magnetic field generation
Self-organized completely kinetic stationary states
Among many others
2011 Summer School
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Equations of State
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We care about the Equation of State (EOS).
Why?
•
In order to
– make inertial fusion work
– model a gas giant planet
– understand the structure
of a white dwarf star
– understand warm dense
matter
•
we need to know how the
density of a material varies
with pressure
•
Here is one theoretical
model of the structure of
hydrogen
Saumon et al., 2000
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MCore/MEarth
The different EOS models for hydrogen directly
impact whether Jupiter is predicted to have a
central dense core or not
20
•
Outlines show range of
models matching Jupiterʼs
properties within 2σ of
observed
•
Cannot yet tell whether
Jupiter has a core
•
The predicted age of
Jupiter is is also sensitive
to the H EOS, which affects
luminosity
15
10
5
0 No core
0
10
20
30
40
MZ/MEarth
[D. Saumon and T. Guillot, Ap. J. 609, 1170 (2004)]
2011 Summer School
Intro to High Energy Density Physics
Adapted from slide by
Bruce Remington
Page 28
EOS results are often shown as the pressure
and density produced by a shock wave
•
This sort of curve is
called a Shock
Hugoniot (or
Rankine-Hugoniot)
relation
Pressure
(GPa)
•
Changing curve
shape comes from
changing structure
•
Other thermodynamic
variables (ε,T) can be
inferred from the
properties of shocks
Compression (density ratio)
Credit: Keith Matzen, Marcus Knudson, SNLA
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Equation of state experiments have been and
will be common at HED facilities
Single-shock and double-shock Omega data
D. Hicks, et al., PHYS. REV. B 79, 014112 (2009)
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Page 30
5 minute stretch
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Radiative Shocks
one topic in radiation hydrodynamics
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Page 32
Most HEDP dynamics
begins with a shock wave
•
•
•
•
If I push a plasma boundary forward at a speed below cs,
sound waves move out and tell the whole plasma about it.
If I push a plasma boundary forward at a speed above cs, a
shock wave is driven into the plasma.
The shock wave heats the plasma it moves through,
increasing cs behind the shock.
Behind the shock, the faster sound waves connect the
entire plasma
Denser,
Hotter
downstream
2011 Summer School
csd > vs
in frame
of shock
Shock velocity, vs
csu < vs
here
Initial plasma
Intro to High Energy Density Physics
upstream
Mach number
M = vs / csu
Page 33
Shock waves become radiative when
•
Radiative energy flux would exceed incoming material energy
flux
σTs4
>
ρous3/2 Upstream
preheated
downstream
•
Where post-shock temperature is
•
The ratio of these energy fluxes is proportional to us5/ρo
•
Implying threshold velocities ….
RTs =
2(! " 1) 2
us
2
(! + 1)
Material
Xe
Xe
CH
Density
0.01 g/cc
10-5 g/cc
0.01 g/cc
Threshold velocity
60 km/s
10 km/s
200 km/s
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Conservation of energy forces the shock wave
to develop complex structure
Shocked xenon layer
Compressed 40x
Traps thermal photons
Preheated region
Thermal photons
escape upstream
Other fun
complications:
Instabilities
Wall shocks
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Intro to High Energy Density Physics
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Radiative shocks are challenging in both
astrophysics and the laboratory
•
Radiative shocks
•
– Radiation alters the structure and
dynamics of the shock
– A radiation-hydrodynamic
phenomenon
– Inherently nonlinear
– Sometimes unstable
– Matching key dimensionless
parameters is what one can
do
•
•
Motivation from astrophysics
– Supernova shocks
– Stellar shocks
– Some accretion phenomena
•
Astrophysical modelers
called for experiments in this
area
Experiments are a major
challenge
– Novel experimental systems
– Need innovation in targets
and diagnostic approaches
Modeling them is difficult
– Widely varying scales
– Radiation transport regimes
– Ionizing media and 3D effects
2011 Summer School
Intro to High Energy Density Physics
Page 36
How to produce radiative shocks
Laser beams launch Be piston
into Xe or Ar gas at > 100 km/s
Gas filled tubes
Piston drives shock
Diagnostics measure plasma
properties
Gold grids provide spatial
reference
Parameters
1015 W/cm2
0.35 µm light
1 ns pulse
600 µm tube dia.
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Intro to High Energy Density Physics
Experiments: Amy Reighard, Tony Visco, Forrest Doss
Page 37
Targets: Korbie Killebrew, Mike Grosskopf,
Trisha Donajkowski, Donna Marion
Researchers are studying these shocks with a
range of diagnostics and simulations
•
Radiographs
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•
Emission
•
Xray Thomson scattering
Intro to High Energy Density Physics
•
Interferometry
Page 38
Data credit: L. Boireau S. Bouquet, F. Doss M. Koenig, C. Michaut, A. Reighard, T. Visco , T. Vinci
Researchers are simulating such shocks too
Level
CRASH 1.0 2D Simulation
Axial vel.
Xe radiograph
(of rotated output)
Radial vel.
Density
Pressure
Te
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Physics
The agreement
here is too good
Page 39
Next directions in the study of radiative shocks
Omega scale:
Determine structure
and dynamics
Both axial and lateral
Create more complex
systems
Reighard Omega experiment
Target for Visco
X-ray Thomson
scattering
experiment
shock
Continuously radiating shock
produces dense xenon layer at
> 30 times initial density.
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Omega has the potential to do
other radiation hydrodynamics
NIF can go further
Intro to High Energy Density Physics
Page 40
Applications of
High Energy Density Physics
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Intro to High Energy Density Physics
Page 41
Why did the US Congress fund HED machines?
•They were developed for inertial confinement fusion (ICF)
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Page 42
In ICF one first compresses the fuel using an
ablatively driven implosion
•
This turns out to be necessary to avoid blowing up the lab
ICF fusion
Capsule
An ablatively driven implosion
Fuel layer is first compressed by shocks.
Then the shell is accelerated inward by high-pressure, low-density corona.
Stagnation creates a central hot spot surrounded by cold dense fuel
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Intro to High Energy Density Physics
Page 43
After compression, one has to make the ICF
fuel burn by fusion
•
Two approaches
Design the central hot spot
so it ignites the fuel
Let the central hot spot be
much smaller and rapidly
ignite the compressed fuel
Options: lasers, particles, slugs
This is the traditional approach
2011 Summer School
This is called fast ignition
Intro to High Energy Density Physics
Page 44
HED experimental astrophysics is emerging
•
New tools enable new science,
and create new sciences
Astronomy: the human eye and brain
Spectroscopy enabled
and created astrophysics
e.g., Hubble
diagram
•
High Energy Density facilities
are new tools …..
2011 Summer School
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Page 45
Laboratory
Laboratoryexperiments
experimentstest
testopacity
opacitymodels
models
that
thatare
arecrucial
crucialfor
forstellar
stellarinterior
interiorphysics
physics
Predictions of solar structure do not
agree with observations (13 σ CZ
problem)
Solar structure depends on opacities that
have never been measured
convective
zone
Challenge: create and diagnose stellar
interior conditions on earth
radiative
zone
Z opacity experiments reach T ~ 156 eV
core
High T enables first studies of transitions
important in stellar interiors
2007 Don Dixon / cosmographica.com
Slide credit: James Bailey
2011 Summer School
transmission
Fe / Mg transmission at T ~ 156 eV
8.0
10.0
12.0
λ (Angstroms)
Intro to High Energy Density Physics
14.0
Page 46
Magnetically-driven z-pinch implosions provide one means to
do studies like this, requiring bright x-ray sources
Current
B-Field
JxB Force
kinetic and electrical energy
electrical energy internal (shock heating)
kinetic energy
x rays
•
•
Initiation
Implosion
Energy: 1.5 MJ x-ray ≈ 15%
of stored electrical
Power: 200 TW x-ray
Stagnation
Slide credit: James Bailey
2011 Summer School
Intro to High Energy Density Physics
Page 47
Opacity and photoionization experiments, relevant to stellar
interiors and accretion powered objects, have been done at
Z and could be done at Omega
opacity sample same charge
states in sun
X-rays
Fe + Mg transmission
Te ~ 156 eV, ne ~ 1022 cm-3
λ
Z
x-ray
source
1-2 MJ
2·1014 W
photoionization sample
radiation effects in
plasma surrounding
black hole
Ne transmission at
Te ~ 25 eV, ne ~ 1019 cm-3
λ
The importance of radiation for creation and diagnosis is a unifying theme
for these very different plasmas
[Jim Bailey, PRL (2007);
and PoP 13, 056301 (2006)]
2011 Summer School
Intro to High Energy Density Physics
Slide credit: James Bailey
Page 48
There are three key dimensionless parameters
for radiative shocks
•
•
•
The ratio radiation flux at the initial postshock temperature to
the incoming material energy flux
4
The upstream optical depth
The downstream optical depth
Cooling layer
Density
Downstream final state
ρf,Tf,pf
Temperature
!T
3
" ou s / 2
Initial post-shock state
ρi,Ti,pi
Upstream ρo,To,po
(Ignoring ion-electron decoupling near the density jump)
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Page 49
Shocks in SNe pass through the regime of our
experiments as they emerge
1987A simulation
•
Xe experiment simulation
Core collapse SNe shock passing through outer layers becomes radiative
– Once radiation ahead of the shock can escape
•
Associated with luminosity burst; radiation escaping to optically thin
region
2011 Summer School
Intro to High Energy Density Physics
A.B. Reighard, Ph.D. Thesis, 2007
Page 50
Ensman and Burrows, ApJ., 393,742-755,1992
The fluid energy equation has a number of
terms that often donʼt matter
•
General Fluid Energy
Equation:
Material Energy
Flux Γm
, $
/
'
u2 '
!$
"u 2
+ E R ) + * + ."u&# +
& "# +
) + pu1 =
!t %
2
2(
(
- %
0
2J • E + Fother • u 2 * • [FR + ( pR + E R )u + Q 2 (3 v • u)]
! ei
~1
" pe
Or
Ideal
MHD
2011 Summer School
Typ.
small
!m
=
PeRad
" rad
!m
" hydro
Smaller
or
Hydro-like
!m
Pe
!m
Re
This enables scaled
astrophysical hydrodynamics
experiments when
Re, Pe, and PeRad are >> 1
Intro to High Energy Density Physics
Page 51
Destruction of clumps in post-shock flow has
been a research area with impact
Chandra data
Well scaled experiment
Klein et al., ApJ 2003
Robey et al., PRL 2002
•
•
•
Experimental results used to help interpret Chandra data from the Puppis
A supernova remnant
Well-scaled experiments have deep credibility
Una Hwang et al., Astrophys. J. (2005)
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Intro to High Energy Density Physics
Page 52
How shock-clump experiments are done
•
… but not in a way that lets
one diagnose details
•
The experiment involves
blast-wave-driven mass
stripping from a sphere
•
Early experiments used Cu
in plastic; recent
experiments use Al in foam
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Intro to High Energy Density Physics
Page 53
Observations of the Al/foam case continued
until mass stripping had destroyed the cloud
•
Hansen et al., ApJ 2007, PoP 2007
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Intro to High Energy Density Physics
Page 54
The stripping is clearly turbulent, consistent
with the necessary conditions
Hansen et al., ApJ 2007
Remaining
Mass (µg)
•
The turbulent model is based
on “Spaldingʼs law of the
wall”, Spalding (1961)
•
Parameters
Re ~ 105 to 106
U ~ 10 km/s
ν ~ 10-5 to 10-6 m2/s
δ ~ Sphere ~ 60 µm radius
•
δ /U ~ 6 ns ~ rollup time (data)
•
Robey/Zhou time is ~ 1 ns
Time (ns)
2011 Summer School
Intro to High Energy Density Physics
Page 55
Perspectives on relativistic HEDP
•
•
The development of Chirped Pulse Amplification in the
1980ʼs soon enabled the production of high-field HEDP
conditions and relativistic electrons
Intense particle beams also are HED media
•
•
Much interesting dynamics occurs
Much of this produces relativistic distributions of particles
– Often exponential in energy
– Energy scales of a few to many MeV
•
Pursuit of acceleration in plasma wakes has led to
discovering organized behavior with the production of
quasi-monoenergetic electron beams
2011 Summer School
Intro to High Energy Density Physics
Page 56
Wakes are common in fluid disturbances
•
•
To experience acceleration on a wake, go wakeboarding or surfing
A wakeboarder can surf the wake on a boat… gaining momentum
http://www.nickandjulz.com/pro/photos/wake/
2011 Summer School
Intro to High Energy Density Physics
Page 57
To accelerate lots of electrons,
take them surfing too
•
Electrons can surf the wake on a pressure pulse in a
plasma
Plasma
Wake
Laser
pulse
Electrons
•
The pressure pulse can be produced by one or more laser
beams or by an electron bunch. This is wakefield acceleration.
2011 Summer School
Credit: LBL OASIS Group
Intro to High Energy Density Physics
Page 58
In 1979, Tajima and Dawson published the
invention of wakefield acceleration
•
A Simple notion
λp
Wake phase velocity
vph = ωpe/kp=ωpeλp/(2π)
Choose ωpe, λp so vph = c
•
Complex implementation
– Through the 1990ʼs this required convincing some plasma
waves to evolve to a final, desired, very nonlinear state
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Intro to High Energy Density Physics
Page 59
In 2002, Pukhov and Meyer-ter-Vehn identified
the “bubble regime”
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Intro to High Energy Density Physics
Page 60
Laser-Plasma Electron Accelerator
Tajima & Dawson, Phys. Rev. Lett. 43, 267 (1979)
INVISIBLE
Gas Jet Fires
about
3 mm
Laser Pulse Focuses
Ionize Gas & Make Wave
Helium Gas Jet
Wave Captures and
Accelerates Electrons
2009 Summer School
slide courtesy Mike Downer, UT-Austin
Intro to High Energy Density Physics
Page 61
First GeV Electron Beam from LWFA
• Laser: a0 ~ 1.46 (40 TW, 37 fs)
• Capillary: D = 312 µm; L = 33 mm
[pC/GeV]
500
1 GeV beam
expt.
250
sim.*
0
0.9
2011 Summer School
Sim
Expt
Q (pC)
25-60
35
E (GeV)
1.0
1.1
dE/E RMS (%)
4
2.5
div. (mrad)
2.4
1.6
1.1
[GeV]
Intro to High Energy Density Physics
Credit: W.P. Leemans et. al, Nature Physics 2 (2006) 696; *Simulation using VORPAL
62
Researchers have developed advanced
diagnostic techniques for plasma accelerators
Magnetic field measurements
of the electron beam
(wavebreaking diagnostic)
2011 Summer School
single shot frequency
domain holography
Intro to High Energy Density Physics
Page 63
Data credits: Mike Downer, Kaluza et al. ( submitted ), Michigan/Texas collaboration, Matlis et al., Nature Physics 2006
Energy Doubling of
42 Billion Volt
Electrons Using
an 85 cm Long
Plasma Wakefield
Accelerator
42 GeV
85GeV
Nature v 445,p741 (2007)
2011 Summer School
Slide Credit: Chan Joshi
Intro to High Energy Density Physics
Page 64
Plasma Accelerator Progress
“Accelerator Moore’s Law”
ILC
Working Machines
Doing physics
E167
E164X
LBNL
RAL
Max.Energy in
Plasma Experiments
2011 Summer School
UCLA
Intro to High Energy Density Physics
LBL
Osaka
Page 65
For a deeper fundamental background in HEDP
•
Come next summer to the next offering of
– Foundations of High Energy Density Physics
•
A thorough introduction to the foundations of this subject
– Taught by one lecturer (me) to provide a continuous
discussion with common notation based on a book
– A two week course
•
Past students have been enthused
– Otherwise I would not be doing this again!
– Contact [email protected]
2011 Summer School
Intro to High Energy Density Physics
Page 66
High-energy-density physics is exciting!
Radiating shocks
Self-organized states
Toward TeV beams
With applications from
supernovae to medicine
2011 Summer School
Credits: Karl Krushelnick, Bedros Afeyan
Intro to High Energy Density Physics
Page 67
Forefront fundamental areas of HEDP
•
High energy density hydrodynamics
– How do the distinct properties of high energy density systems alter
hydrodynamic behavior?
•
Radiation-dominated dynamics and material properties
– What are the unique properties of radiation-dominated HED
plasmas?
•
Magnetized HED dynamics
– How do magnetic fields form, evolve, and affect the properties of
high energy density plasmas?
•
Nonlinear optics of HED plasmas
– How does high-intensity coherent radiation alter the behavior of
high energy density plasmas?
•
Relativistic high energy density plasma physics
– How do plasmas with relativistic temperatures or relativistic flows
behave?
•
Warm dense matter physics
– What are the state, transport, and dynamic properties of warm
dense matter?
2011 Summer School
Intro to High Energy Density Physics
Page 68