high harmonic generation in ionization of magnetically dressed atoms
DESCRIPTION
APS Centennial Meeting Atlanta 1999 DAMOP Undergraduate Research Symposium. High Harmonic Generation in Ionization of Magnetically Dressed Atoms. Robert E. Wagner Freshman Intense Laser Physics Theory Unit Illinois State University. www.phy.ilstu.edu/ILP. Acknowledgment. - PowerPoint PPT PresentationTRANSCRIPT
High Harmonic Generation in Ionization of Magnetically
Dressed Atoms
Robert E. Wagner
Freshman
Intense Laser Physics Theory Unit
Illinois State University
APS Centennial Meeting Atlanta 1999 DAMOP Undergraduate Research Symposium
Undergrad researchers:P. Peverly, electron dynamics
J. Braun, quantum simulations
J. Csesznegi, graphics
T. Shepherd, animations
Advisors: Profs. Q. Su, R. Grobe
Support:
National Science Foundation
Research Corporation
ISU Honor’s Program
Scattered Light Spectra in Ionization
L
? ? ?
I()
L
1
L
2
H c4 c2 (p A(r, t) / c) 1/ r
A(r, t)f()c E
L
sin(Lt ky)ex 1
2rB
Relativistic Newton Equations
• RK-4 variable step size simulation
• Spectra of scattered light
Non-relativistic regime: E < 1 a.u.L
aser
Int
ensi
ty
= L L + M a
(L + M = odd)
10-9
10-5
0 1 2 3
I z (
) [a
.u.]
[a.u.]
E0 = 0.332 a.u.
10-9
10-5
0 1 2 3
I z (
) [a
.u.] E
0 = 0.331 a.u.
10-9
10-5
10-1
0 1 2 3
I z (
) [a
.u.]
10
30
-21
01
21
-32
41
-12
32
-23
03
23
LM
E0 = 0.16 a.u.
= L L (L = odd) Shifted atomic lines
L
Rapid ionization
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Relativistic regime: E > 1 a.u.L
aser
Int
ensi
ty
= L L (L = even + odd)
L 1E2
4L2 c2
1
L
10-8
10-6
10-4
10-2
0 0.5 1 1.5 2
I x (
) [a
.u.]
[a.u.]
E0 = 10 a.u.
10-4
10-3
10-2
10-1
100
0 0.5 1 1.5 2
I x (
) [a
.u.]
[a.u.]
E0 = 30 a.u.
Relativistic redshift
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Magnetically dressed atomsL
aser
Int
ensi
ty
Perturbative regime: E < 0.1 a.u.
Non-rel. strong field: 0.1 < E < 1.0 a.u.
Relativistic magnetic resonances: E > 1.0 a.u.
Non-rel. Perturbative Regime: E < 0.1
2
2
a2
2 = Cyclotron frequency
(3,1,1)
L L + M + + N - (L + M + N = odd)
10-11
10-9
10-7
10-5
0 1 2 3
I z (
) [a
.u.]
[a.u.]
Analytically Soluble ModelH
1
2p
1
2cr B
2
E sin(Lt)
Iy (,) Cy (m1,m2 )2 ( m1 m2L )m1, m2
C y(m1,m2 )
E22
c3 (2 L2 ) 2 J' m1
Ec(2 L
2 )
Jm2
EcL(2 L
2 )
LJ' m2
EcL (2 L
2 )
Jm1
Ec(2 L
2 )
2
10-8
10-6
10-4
10-2
0 0.5 1 1.5
I y (
) [a
.u.]
[a.u.]
+ analytical — exact
Relativistic Magnetic Resonances
Typical Orbit
Maximum displacement
How do the spectra evolve as a function of
-2000
0
2000
-4000 -2000 0
y [a
.u.]
x [a.u.]
101
102
103
104
0 0.2 0.4 0.6 0.8 1
x m
ax [
a.u.
]
[a.u.]
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Summary-=0 -> main features understood
- Analytical model -> retardation effects in spectra
- Novel rel. resonances enhance higher harmonics
- Challenges ahead: coherence, quantum aspects...
www.phy.ilstu.edu/ILP
R. E. Wagner, Q. Su and R. Grobe, Phys. Rev. A (submitted)