8/4/2019 L.O. Silva-Particle Acceleration & Relativistic Astrophysics in the Lab
1/45
Particle acceleration &relativistic astrophysics in the lab
G
oLP/IF
PN
Institu
to
Superior
T
cnico
L. O. Silva | ELI Scientific Challenges, April 26 2010
8/4/2019 L.O. Silva-Particle Acceleration & Relativistic Astrophysics in the Lab
2/45
L. O. Silva | ELI Scientific Challenges, April 26 2010
Acknowledgments
S. F. Martins, F. Fiza, J. Vieira, J. Martins,M. Marti, R. A. Fonseca
Work in collaboration with:
F. Tsung, J. Tonge, J. May, W. B. Mori (UCLA)
Simulation results obtained at epp and IST Clusters (IST),
Dawson Cluster (UCLA), Franklin (NERSC), Intrepid(Argonne), and Jugene (FZ Jlich)
8/4/2019 L.O. Silva-Particle Acceleration & Relativistic Astrophysics in the Lab
3/45
L. O. Silva | ELI Scientific Challenges, April 26 2010
Contents
Laser e- acceleration
Boosted frame simulations 10 PW laser
High brilliance betatron radiation
Gamma ray beams
Relativistic beams for astrophysics
Relativistic shocks
Conclusions
8/4/2019 L.O. Silva-Particle Acceleration & Relativistic Astrophysics in the Lab
4/45
L. O. Silva | ELI Scientific Challenges, April 26 2010
Contents
Laser e- acceleration
Boosted frame simulations 10 PW laser
High brilliance betatron radiation
Gamma ray beams
Relativistic beams for astrophysics
Relativistic shocks
Conclusions
8/4/2019 L.O. Silva-Particle Acceleration & Relativistic Astrophysics in the Lab
5/45
L. O. Silva | ELI Scientific Challenges, April 26 2010
Particle accelerators: rich science and applications
Adapted from Tom Katsouleas (Duke)
LargeVerified Standard Model of ParticlePhysics
W, Z bosons
Quarks, gluons and quark-gluonplasma
Asymmetry of matter and anti-matter
In pursuit of the Higgs boson
CompactMedicine
cancer therapy, imaging
Industry
lithography
Light sources (synchrotrons)bio imaging
condensed matter science
International Linear Collider
8/4/2019 L.O. Silva-Particle Acceleration & Relativistic Astrophysics in the Lab
6/45
L. O. Silva | ELI Scientific Challenges, April 26 2010
Particle accelerators
High Energy
HighLuminosity
High BeamQuality
Low Cost
L = fN2
/4xy
/ 0.1% 10% n yy < 1 mm mrad
[event rate]
[low energy spread] [low emittance]
[1/10 of 1010!/TeV]Gradients > 100 MeV/m Efficiency > few %
8/4/2019 L.O. Silva-Particle Acceleration & Relativistic Astrophysics in the Lab
7/45
L. O. Silva | ELI Scientific Challenges, April 26 2010
Recent achievements in laser-plasma accelerators
Guiding in plasma channels and ~1 GeV e- beams
Leemans et al, Nat. Phys. (2006)
Self-guided propagation and self-injected electrons (>1 GeV)
Hafz et al, Nat. Photonics (2008); Kneip et al, PRL (2009); Froula et al, PRL (2009);Clayton et al, submitted [1.4 GeV in 1.3 cm @ 1018 cm-3]
Controlled all-optical injection of monoenergetic electron beams
Faure et al, Nature (2006)
Beam loading in nonlinear wakes
Tzoufras et al (2008); Rechatin et al (2009)
Intense incoherent radiation (betatron x-rays & undulator radiation)
Rousse et al, PRL (2004); Kneip et al(submitted); Froula et al(in preparation) &H.-P Schlenvoigt et al, Nat. Phys. (2004); M. Fuchs et al, Nat. Phys. (2009)
8/4/2019 L.O. Silva-Particle Acceleration & Relativistic Astrophysics in the Lab
8/45
L. O. Silva | ELI Scientific Challenges, April 26 2010
Recent progress has put plasma accelerationat the forefront of Science
8/4/2019 L.O. Silva-Particle Acceleration & Relativistic Astrophysics in the Lab
9/45
L. O. Silva | ELI Scientific Challenges, April 26 2010
Tech developments have triggered recent progresses
09 Peak laser intensity ~ 1022 W/cm2 09 Peak computing power > 1 Tflop/s
Mourou, Tajima, Bulanov (2006) Source: top500.org
8/4/2019 L.O. Silva-Particle Acceleration & Relativistic Astrophysics in the Lab
10/45
New Features in v2.0
Bessel Beams
Binary Collision Module
Tunnel (ADK) and Impact Ionization
Dynamic Load Balancing PML absorbing BC
Optimized higher order splines
Parallel I/O (HDF5)
Boosted frame in 1/2/3D
osiris framework
Massivelly Parallel, Fully RelativisticParticle-in-Cell (PIC) Code
Visualization and Data Analysis Infrastructure
Developed by the osiris.consortium! UCLA + IST
OSIRIS 2.0
Ricardo Fonseca: [email protected] Tsung:[email protected]
http://cfp.ist.utl.pt/golp/epp/http://exodus.physics.ucla.edu/ L. O. Silva | ELI Scientific Challenges, April 26 2010
8/4/2019 L.O. Silva-Particle Acceleration & Relativistic Astrophysics in the Lab
11/45
L. O. Silva | ELI Scientific Challenges, April 26 2010
OSIRIS strong scaling up to ~300k CPUs
! Spatial domain decomposition! Local field solver! Minimal communication! Dynamic Load Balancing
Optimize scalability and tap new hardwares
New hardware features
SIMD units
tailored code already in production
GPUs
CUDA development (test PIC code)
PowerXCell
1
10
100
104
105
Spe
ed
up
CPUs
JUGENEGermany
8/4/2019 L.O. Silva-Particle Acceleration & Relativistic Astrophysics in the Lab
12/45
L. O. Silva | ELI Scientific Challenges, April 26 2010
Can LWFA reach the energy frontierwith the next generation of lasers?
!! ! ! ! !! ! ! ! ! ! !
! ! ! ! ! ! ! ! ! ! ! ! ! !! ! ! ! ! ! ! ! ! ! ! !
!
! ! ! ! ! ! ! ! ! ! ! ! ! !! ! ! ! ! ! ! ! ! ! ! ! !
! ! ! ! ! ! ! ! ! ! ! ! !! ! ! ! ! ! ! ! ! !
! ! ! ! ! ! ! ! ! ! !! ! ! ! ! ! ! ! ! ! ! ! ! !
! ! ! ! ! ! ! ! ! ! !! ! ! ! ! ! ! ! ! ! ! ! !! ! ! ! ! ! ! ! ! ! !
! ! ! ! ! ! ! ! ! ! ! !! ! ! ! ! ! ! ! ! ! ! !! ! ! ! ! ! ! ! ! ! ! ! ! ! !
! ! ! ! ! ! !
! ! ! ! ! ! ! ! ! ! ! ! !! ! ! ! ! ! ! ! ! ! ! ! ! ! ! !
! ! ! ! ! ! ! ! ! ! ! ! ! !!
!"#$%%&'()"
*+,-.)/&0."1234
!""#$%&'()*
+,-'/#56(%(789+--: .;0.
!""#$%&'()+
+,-'/#56(%(789+--:.;0.
!""#$%& '(),
+,-'/#56(%(789+--:.;0.
-".%&'()/+01!+?@/&0%$6/
9+--:.;0.
*2-345"67/+01
!+?@/&0%$6/
,%&"5%&0..;0.
*2(?=@AB#
*+?=*CB#
*+?=*CB#
>DEFDG$%G#D$H$%#$IJ#%&B'6D5D$H
K0"$D6)FH#D6#
% 'GL)M
'66%5%&'$D"G
N;O=N&'H
E%G%&'$D"G
-5'#(')FH#D6#
3PQ
*2?
C2?
,22?
+0+22(< =*7>?=*2B#8))5D6'$D"G#
E0(%/#;%&)F@$(0/G$#&%H0&'/)$&%"#$/6#/"I
!%'(=)J5#%#.D$6FH'&L
C2?
! ! ! ! ! ! ! ! ! ! ! ! !
!!
!!!!
!
!!!
!!!
!! ! ! !!!!!!!!!!!
!!
!!!!
8/4/2019 L.O. Silva-Particle Acceleration & Relativistic Astrophysics in the Lab
13/45
L. O. Silva | ELI Scientific Challenges, April 26 2010
Limits to energy gain in LWFA
E= eEzLacc
Diffractionlaser pulse diffracts inscale ofZr (Rayleigh length) ~ few mm
Depletionlaser pulse looses its energy to the plasma in Ldeplfor small a0, Ldepl >> Ldph ; for a0 > 1, Ldepl ~ Ldph
TK & JMD 83
Recenin using
laser-p
ticles to high e
nergie
to whichlinear a
ccelerators
1limited.
The beat-wave ac
celerator2
proposedby Dawso
n and Tajima to
excite larg
tude electrostat
ic plasma waves
which can accele
ra
particles.' Whe
reas particles i
n the beat-wave
accel-
erator can g
ain onlya finite
amount of energy
before
they become out
of phasewith the
beat wave, by i
ntro-
ducing aperpend
icular magnetic
field the partic
les
are deflected acros
s the wave front
therebypreventi
them from outrun
ning thewave. T
he particles may
b
accelerated to a
rbitrarily high
energy as they r
id
across the wave'
fronts like surfers
cuttingacross
face ofan ocean
wave (see Fig. 1
).
-B AB, z
/ yFig. 1 An
electrontrapped
by a pot
ing at Vph sees
an electric
which accelerates
it across
Sugiharaand Midzu
no3 and
shown that class
ical particles
dicularly propag
ating electros
ted until they d
e-trap near t
is letter we con
sider t
when theE x B ve
i.e., E> B
comp
Dephasingelectrons overtake accelerating structurein Ldph ~ 10 cm/n0 [1016 cm-3]
v ~ vgroup laser
v ~ c
8/4/2019 L.O. Silva-Particle Acceleration & Relativistic Astrophysics in the Lab
14/45
Blow-out regime of laser wakefield acceleration
L. O. Silva | ELI Scientific Challenges, April 26 2010
8/4/2019 L.O. Silva-Particle Acceleration & Relativistic Astrophysics in the Lab
15/45
L. O. Silva | ELI Scientific Challenges, April 26 2010
Match laser spot size tobubble radius
Linear focusingforce
Electric fields created by laser pulse
Phenomenological theory based on physical picture
W. Lu et al. PR-STAB (2007)
Longitudinal
Ezmaxa0
kpR kpW0 = 2 a0
Letch > Ld
cFWHM > 2R/3Ld
2
3
20
2p
R
Matched laser parameters
Transverse
kpR 2a0
Linear acceleratinggradient
For maximum energy gain:trapped e- dephasing before pump depletion
Letch c2
0/2
pFWHM
8/4/2019 L.O. Silva-Particle Acceleration & Relativistic Astrophysics in the Lab
16/45
L. O. Silva | ELI Scientific Challenges, April 26 2010
W0 =3
2cFWHM
np[1018 cm3] 3.71
a30
P[TW]
0[m]
0.8
2
FWHM[fs] 53.22
0[m]
0.8
2/3
[J]
a20
1/3
Lacc[cm] 14.09[J]
a30
q[nC] 0.17
0[m]
0.8
2/3([J] a0)
1/3
E[GeV] 3
[J]
a20
0.8
0[m]
2/3
Different regimes for the LWFA
* S. Gordienko and A. Pukhov PoP (2005)** W. Lu et al. PR-STAB (2007)
Main goalMaximize
electron energy
Efficiency
0.52/a019%
Typical a0 2nc/np (nc/np)
1/5 2 3
Maximum electron energy
8/4/2019 L.O. Silva-Particle Acceleration & Relativistic Astrophysics in the Lab
17/45
L. O. Silva | ELI Scientific Challenges, April 26 2010
Parameter range for 250 J laser system
Laser
Plasma
e- Bunch
a0
Spot [m]
Duration [fs]
Density [cm-3]
Length [cm]
Energy [GeV]
Charge [nC]
* S. Gordienko and A. Pukhov PoP (2005)** W. Lu et al. PR-STAB (2007)
Simulationtime [days in
512CPUs]
8/4/2019 L.O. Silva-Particle Acceleration & Relativistic Astrophysics in the Lab
18/45
L. O. Silva | ELI Scientific Challenges, April 26 2010
Boosted Frames in LWFA simulations
L
aboratoryFrame Resolution gains
Particles
Time steps
Total
Time step (1 + )
Resolution (1 + )
Plasma
contraction
Total time (1 +
)
2(1 + )2BoostedFrame
J.-L. Vay, PRL 98, 130405 (2007)
8/4/2019 L.O. Silva-Particle Acceleration & Relativistic Astrophysics in the Lab
19/45
L. O. Silva | ELI Scientific Challenges, April 26 2010
+3GeV self-injection in strongly nonlinear regimeExtreme blowout a0=53
Laboratory frame3000x256x256 cells
~109 particles105 timesteps
x2
[m]
ElectronEnergy[GeV]
90
60
30
0
3
2
1
0
x1 [ m]
806040200
x1 [ m]
806040200
x1 [ m]
806040200
x1 [ m]
80604020010
-3
10-1
e-density[1
.5e19cm
]-3
101
10
1
S.F. Martins et al, Nature Physics (2010)
8/4/2019 L.O. Silva-Particle Acceleration & Relativistic Astrophysics in the Lab
20/45
L. O. Silva | ELI Scientific Challenges, April 26 2010
~300x fasterthan lab simulation
ElectronEnergy
Lab[GeV]
2
6
10
14
130001250012000
600050004000
x2
Boost[m]
x1 Boost [m]
x1
Boost [m]
x1
Boost [m]
x2
Boost [m]
100
200
300
400
400
200
200
300
300
2400
0
1200
Density
e-Energy
Lab[GeV]
-3
Density
[2.7e17cm
]-1
80
40
0
5
3
1
10
-2
10
x3
Boost [m]
Laser
pulse
Accelerating
electron beam
+10GeV self-injection in nonlinear regimeControlled self-guided a0=5.8
Boosted frame7000x256x256 cells
~109 particles3x104 timesteps
=10
8/4/2019 L.O. Silva-Particle Acceleration & Relativistic Astrophysics in the Lab
21/45
L. O. Silva | ELI Scientific Challenges, April 26 2010
10
20
30
40
0 1 2 3 4 5
Ez
[GV/cm]
x1
Boost [m]
0.1
0.0
-0.1
6000400020000
Distance [m]
Energy[GeV]
+40GeV with externally injected beamsChannel guided a0=2
Boosted frame8000x128x128 cells
~5x108 particles2x105 timesteps
=10
~300x fasterthan lab simulation
8/4/2019 L.O. Silva-Particle Acceleration & Relativistic Astrophysics in the Lab
22/45
L. O. Silva | ELI Scientific Challenges, April 26 2010
Regime comparison and fine-tuning
7000x256x256 cells~109 particles
3x104 timesteps=10
8/4/2019 L.O. Silva-Particle Acceleration & Relativistic Astrophysics in the Lab
23/45
Particle accelerators & plasmas
High Energy
HighLuminosity
High BeamQuality
PolarizedBeams
Low Cost
L. O. Silva | ELI Scientific Challenges, April 26 2010
8/4/2019 L.O. Silva-Particle Acceleration & Relativistic Astrophysics in the Lab
24/45
L. O. Silva | ELI Scientific Challenges, April 26 2010
Contents
Laser e- acceleration
Boosted frame simulations 10 PW laser
High brilliance betatron radiation
Gamma ray beams
Relativistic beams for astrophysics
Relativistic shocks
Conclusions
8/4/2019 L.O. Silva-Particle Acceleration & Relativistic Astrophysics in the Lab
25/45
L. O. Silva | ELI Scientific Challenges, April 26 2010
Applications for LWFA beams
LINAC
undulator
100m
1km
1cm
E > 10 GeV
B ~ 1 T
LightSources(FEL)
Plasm
abased
Ultra shortaccelerating
structure
Undulator likemotion in ion
channel
8/4/2019 L.O. Silva-Particle Acceleration & Relativistic Astrophysics in the Lab
26/45
L. O. Silva | ELI Scientific Challenges, April 26 2010
Betatron radiation in plasma wakefield acceleration
Ultra shortaccelerating
structure
S. Wang et al, PRL (April 2002)
I ~ 1019 photons/s 0.1 % BW mm2 mrad2@ 6 keV
8/4/2019 L.O. Silva-Particle Acceleration & Relativistic Astrophysics in the Lab
27/45
Scaling for multi-PW lasers (300 J class lasers)
Wigglerstrength
CriticalFrequency
RadiatedPower
Radiated
Energy
* W. Lu et al. PR-STAB (2007)** E. Esarey et al. PRE (2002)
3a2
r/c
remec22
a2
Ne/3
Power lacc/c
kpr0
0/p
= p/2
kpr03/2
p/0 0
= r0/W0
26([300 J])1/6(0[m]/a0)1/12
580([300 J]/a20)1/3(0[m])
1/60
2.8 107([300 J])5/6(0[m])5/12a1
/6
0 0
2.52([300 J])1/3a4/30
(0[m])1/3kW
32([300 J])2/3a5/30
(0[m])1/6GW
372([300 J])4/3a2 30
(0[m])1/3J
53 2([300 J])5/3a1/30
(0[m])1/6mJ
...
...
...
L. O. Silva | ELI Scientific Challenges, April 26 2010
8/4/2019 L.O. Silva-Particle Acceleration & Relativistic Astrophysics in the Lab
28/45
L. O. Silva | ELI Scientific Challenges, April 26 2010
Particle tracking in OSIRIS
Technically challenging
Subset of ~103 particles in ~109
Storing information for every particlenot feasible
104 iter. " 109 part. ~ 500 TB
Relevant physics associatedwith small subset of particles
Record detailed 7D phase-spaceof interesting particles
follow interestingparticles
tag all particles
8/4/2019 L.O. Silva-Particle Acceleration & Relativistic Astrophysics in the Lab
29/45
>10GeV simulation for next generation lasers
Total radiated energy ~ 80 mJ
Typical photon energy ~ 0.1-1 MeV
Typical # of photons ~ a few 1011
Beam divergence ~ Kwiggler/ ~ 2 - 5 mrad
Ebeam ~ 10 GeV
nplasma ~ 1017 cm-3
r0 ~ rbeam ~ 5 m
+10 GeV blowout LWFA stage
Radiated Power
P =1
12
e2
c34
pr2
02
Typical Frequency
c =3
4c2r0
2
p
Kwiggler ~ 52
Full Particle Tracking & Radiation
L. O. Silva | ELI Scientific Challenges, April 26 2010
8/4/2019 L.O. Silva-Particle Acceleration & Relativistic Astrophysics in the Lab
30/45
L. O. Silva | ELI Scientific Challenges, April 26 2010
Collimated radiation beam for >12 GeV e- beam
measured beam angulardivergence (/2):in x2 = 0.64 mradin x3 = 0.61 mrad
26.5 cm 25.8 cm
8/4/2019 L.O. Silva-Particle Acceleration & Relativistic Astrophysics in the Lab
31/45
L. O. Silva | ELI Scientific Challenges, April 26 2010
X-rays to -rays betatron radiation
spectral intensity at center point
zoom
8/4/2019 L.O. Silva-Particle Acceleration & Relativistic Astrophysics in the Lab
32/45
L. O. Silva | ELI Scientific Challenges, April 26 2010
Contents
Laser e- acceleration
Boosted frame simulations 10 PW laser
High brilliance betatron radiation
Gamma ray beams
Relativistic beams for astrophysics
Relativistic shocks
Conclusions
8/4/2019 L.O. Silva-Particle Acceleration & Relativistic Astrophysics in the Lab
33/45
Gamma Ray Bursters
Relativistic colliding flows present in many astro scenarios
N. Gehrels, L. Piro and P. J. T. Leonard, Scientific American, Dec. 2002, p. 89
L. O. Silva | ELI Scientific Challenges, April 26 2010
8/4/2019 L.O. Silva-Particle Acceleration & Relativistic Astrophysics in the Lab
34/45
Plasma instabilities critical to shock formation and field structure
B-fields generated by currentfilamentation/Weibel in GRBs[Medvedev & Loeb, Gruzinov & Waxman, 99, Silva et al, 03]
Fields in relativistic shocks
are mediated by Weibel/current
filamentation generated fields
[Spiktovsky 08, Martins 09]
Shockfront
|B|2
density
L. O. Silva | ELI Scientific Challenges, April 26 2010
8/4/2019 L.O. Silva-Particle Acceleration & Relativistic Astrophysics in the Lab
35/45
Fields in shock Fermi acceleration B-field generation/amplification
Ab initio Fermi acceleration
determined by structure of the fields
in the shock front
[Spitkovsky 08, Martins et al, 09]
B-field amplification in
upstream region via non-
resonant Bell instability[Bell 04]
-
-
L. O. Silva | ELI Scientific Challenges, April 26 2010
8/4/2019 L.O. Silva-Particle Acceleration & Relativistic Astrophysics in the Lab
36/45
8/4/2019 L.O. Silva-Particle Acceleration & Relativistic Astrophysics in the Lab
37/45
z [m]x [m]
100
100
150
150
50
50
0
40
80
y [m]
150 0 20 40 60 8010050
150
100
50
y[m]
150
100
50
y[m]
x [m] z [m]
Density[2.7e17cm-3]
3.0
2.0
1.0
0.0
MagneticField[T]
20
10
0
-10
-20
100
10
1
Density
Magnetic Field
Beam is charge neutral = no blow-out
ElectronsPositrons
Beam filamentation and B-field generation
L. O. Silva | ELI Scientific Challenges, April 26 2010
8/4/2019 L.O. Silva-Particle Acceleration & Relativistic Astrophysics in the Lab
38/45
Standard
5x beam temperature
10x plasma density
2 4 6 8 10
Distance x [cm]
Log
(
10
B
B
0
2 4 6 8Distance x [10 c/ ]p
3
-0
-1
-2
-3
-4
-5
WeibelinstabilityLinear stage
Beam length< p
Transition from purely transverse to mixed mode
Beam filamentation and B-field generation
nb=nplasma
Beam length~ p
L. O. Silva | ELI Scientific Challenges, April 26 2010
8/4/2019 L.O. Silva-Particle Acceleration & Relativistic Astrophysics in the Lab
39/45
Radiation is direct evidence for scattering in Weibel turbulence
n
v
t
d2I
dd=
e2
4c
n [(n )]
(1 n )2ei(tn.r(t)/c)
dt
2
100 101 102 103 104
Var1
106
107
108
Selected
Va
riables
!/!p
P(!)
!!!!
-1
!!-2
Synthetic radiation spectrum
dI/d
L. O. Silva | ELI Scientific Challenges, April 26 2010
8/4/2019 L.O. Silva-Particle Acceleration & Relativistic Astrophysics in the Lab
40/45
H. Takabe
H. Takabe et al, PPCF 50, 124057 (2008)
Formation and propagationof Weibel mediated
collisionless shocks
Recent developments Youichi Sakawa et al, HEDLA (2010), submitted to PRL (2009)
8/4/2019 L.O. Silva-Particle Acceleration & Relativistic Astrophysics in the Lab
41/45
Numerical Parameters
x kp = 0.5 - 1.5
z kp = 0.5 - 1.5
Particles per cell = 64 # particles = 5x109
# time steps = 105
Ignitionlaser
0 = 1m
I0 = 5x1019 - 5x1021 Wcm-2
plane polarized
56 m x 16 m
ne0 = 100 nc
mi/me = 3672 (D+)
Ti0 = Te0 = 100 eV
Physical Parameters
Laser
Plasma
F. Fiza et al, in preparation (2010)L. O. Silva | ELI Scientific Challenges, April 26 2010
8/4/2019 L.O. Silva-Particle Acceleration & Relativistic Astrophysics in the Lab
42/45
Magnetic field
Electron density
Ion phase-space
Current filamentation instabilityleads to thermalization/slow down
of incident beam
reflected ions
shock front
hot region
strong mass build-up/compression
~ 20 c/pi
L. O. Silva | ELI Scientific Challenges, April 26 2010
8/4/2019 L.O. Silva-Particle Acceleration & Relativistic Astrophysics in the Lab
43/45
electron density
vreflected ions = 0.2 cvshock= 0.1 c
vhole boring = 0.07 c
laser
vshock
vreflected ionsvhole boring
n2
n1
hb =
nc
2ne
Zm
M
I2
1.37 1018
1/2= 0.07*
shock =(1 + add)
2d 1
1 + d + ad(2
d 1)
0.1n2
n1
=add + 1
ad 1 3
**
~ 100 c/pi
L. O. Silva | ELI Scientific Challenges, April 26 2010
8/4/2019 L.O. Silva-Particle Acceleration & Relativistic Astrophysics in the Lab
44/45
L. O. Silva | ELI Scientific Challenges, April 26 2010
Contents
Laser e- acceleration
Boosted frame simulations 10 PW laser
High brilliance betatron radiation
Gamma ray beams
Relativistic beams for astrophysics
Relativistic shocks
Conclusions
8/4/2019 L.O. Silva-Particle Acceleration & Relativistic Astrophysics in the Lab
45/45
L. O. Silva | ELI Scientific Challenges, April 26 2010
Conclusions
+ 40 GeV beams with 250 J laser system
New laser systems in the 10 PW range able to explore full range of LWFAscenarios
From high charge multi-GeV beams to externally injected 40 GeV beams
High brilliance gamma-ray beams from betatron radiation
Betatron radiation generated can reach novel parameters not achievable withother machines
Gamma-ray beams from betatron radiation with ~ 10 GeV beams
Relativistic beams/flows for astrophysics
Beams appropriate to probe basic processes relevant in relativisticastrophysics
Ability to drive relativistic shocks in the laboratory