Bayramian, A

Bibeau, C

Caird, J

Cross, R

Dunn, J

Ebbers, C

Erlandson, A

Froula, D

Liao, Z

Meier, W

Molander, B

Schaffers, K

Telford, S

Caird, J.

Bayramian, A.

Bibeau, C.

Cross, R.

Dunn, J.

Ebbers, C.

Erlandson, A.

Froula, D.

Liao, Z.

Meier, W.

Molander, B.

Schaffers, K.

Telford, S.

UNT (University of North Texas) Digital Library

UCRL-CONF-221983 Mercury: A High Repetition RateLaser for High Energy DensityPhysics J. Caird, A. Bayramian, C. Bibeau, R. Cross, J. Dunn, C. EbbersA. Erlandson, D. Froula, Z. Liao, W. Meier, B. Molander,K. Schaffers, S. TelfordJune 12, 200629th European Conference on Laser Interaction with MatterMadrid, SpainJune 11, 2006 through June 16, 2006Disclaimer   This document was prepared as an account of work sponsored by an agency of the United States Government. Neither the United States Government nor the University of California nor any of their employees, makes any warranty, express or implied, or assumes any legal liability or responsibility for the accuracy, completeness, or usefulness of any information, apparatus, product, or process disclosed, or represents that its use would not infringe privately owned rights. Reference herein to any specific commercial product, process, or service by trade name, trademark, manufacturer, or otherwise, does not necessarily constitute or imply its endorsement, recommendation, or favoring by the United States Government or the University of California. The views and opinions of authors expressed herein do not necessarily state or reflect those of the United States Government or the University of California, and shall not be used for advertising or product endorsement purposes.  RJB/VGMercuryMercury: A High Repetition Rate Laser for High Energy Density Physics 29th European Conference on Laser Interaction with MatterMadrid, Spain, June 11 - 16, 2006John Caird, Andy Bayramian, Camille Bibeau, Rick Cross, Jim Dunn, Chris Ebbers, Al Erlandson, Dustin Froula, Zhi Liao, Wayne Meier, Bill Molander, Kathleen Schaffers, and Steve TelfordLawrence Livermore National LaboratoryLivermore, CaliforniaThis work was performed under the auspices of the U. S. Department of Energy by the University of California, Lawrence Livermore National Laboratory under Contract No. W-7405-Eng-48.Gas CooledAmplifier withCrystalline SlabsThe  Mercury LaserPockels cellOutput telescopeSystem controls55100Energy (J) (@ 1 w)StatusGoals6Soon0.523-1010 Hz6.55>1500.52/0.353-101010Beam quality (xDL)Bandwidth GHzWavelength (mm)Pulse length (ns)PRF (Hz)Efficiency (%)0.0 0.2 0.4 0.6 0.8 1.0 1.2 1.4110100Number of Shots (x 105)Output Near Field Output FarField (4 XDL)Output Energy(J)Mercury demonstrated 550 W for > 105 shotsJune 0555 J at 10 HzOctober 0565J at 5 Hz1.45 1.46Mercury uses advanced state-of-the-art technologyDiode pump arrays• Commercialization• 70% EfficiencySolid-state amplifier• Improved Yb:SFAP quality • 12 cm diameter growthHelium gas cooling• Low thermal wavefront • 4 hours operation @ 10 HzBroadband Front End• Fiber based design• 340 mJ demonstratedFrequency Converter• 5.5 x 8.5 cm2 YCOB slabs• Scalable cooling designAdaptive Optic• High resolution sensor• 41 act. bi-Morph mirror227 W green generated550 W infrared generatedAssess perf.2 KDP43w Conversion crystalsBetter YCOB3 YCOB/4 KDP22w Conversion crystalsOnline Commissioned1 DMWavefront control222Amplifiers2w/3w2w2w/3wConversionQualifiedOffline  >150  Bandwidth (GHz @ 1w)3-1515 3-10 Pulse-shaping (ns)<56 @ 55J (80%)5Beam quality (xDL)109109108Diode reliability (shots)>64.510Efficiency (%)10 10 10Rep-rate (Hz)>6055  (65 J)100Energy (J)Laser Performance0.12% 0.12% <1% - Cooling uniformity (rms)360 360288Diode tiles (120 W/bar)28 1414Amplifier slabs (4x6 cm)End FY06PresentGoalComponentsCompletedMercury will reach performance goals in 2006-2007.  User facility activation also expected in 2007  RJB/VGMercuryA HED target shooting experimental facility using Mercury is highly synergistic with IFE goals• Target experiment requirements are similar• HED physics for IFE• X-ray source for diagnostic calibrations• Laser component lifetimeRJB/VGMercuryA high repetition rate User Facility has numerous advantages• Accurately measure statistical variability of phenomena• Signal to Noise (S/N) enhancement by signal averaging• Measure entire parametric variation in a single run, e.g.,– Drive energy– Pulse – diagnostic delay– Pulse duration– Gas pressure (jet)– Target composition, or gas mixture (e.g., He-H ratio)– Target aspect ratioRepetitively pulsed systems are the way for the futureRJB/VGMercuryMercury capability will increase in phases2w/3w (long pulse), 0.8,1.0,1.6,2.0 micron short pulse2w/3w2wFrequency conversionYesYes – 2 long pulsesYes - 2 long pulsesPump/probe optionNew room + Short pulse systemsmall chamber then new roomIn lab small chamber, CY2006Target chamberSingle, 0.1,1,3,5,10, burst Single, 0.1,1,3,5,10, burst Single, 0.1,1,3,5,10, burst Shot rate (Hz)Near field / Far field / Wavefront / Energy / Temporal / autocorrNear field / Far field / Wavefront / Energy / TemporalNear field / Far field / Wavefront / Energy / TemporalDiagnostics250 GHz to >33 THz250 GHz20 MHz BandwidthTBD1.047 um 1.047 um WavelengthGoal:4.2x7.2 cm beam & 1 meter lens80% energy in 0.05 mm dia.Goal:4.2x7.2 cm beam & 1 meter lens80% energy in 0.25 mm dia.40% energy in .05 mm dia. Est. 4.2 x 7.2 cm beam & 1 meter lens96% energy in 0.525 mm dia.80% energy in 0.325 mm dia.20% energy in 0.05 mm diaEnergy in bucket (100% diameter and  80% diameter)30 fs - 10 ps3-15 ns +/- 10% ampl fluctuations15 ns +/- 10% ampl fluctuationsPulse length and shape<100 J +/- 5%100 J +/- 5%50 J +/- 5% (70-100 J next quarter)Energy and rmsMercury short pulse option + new roomMercury + adaptive optics and FE w/bandwidthMercury incurrent state Define in detailPhase 3 – 2007-09Phase 2 – 2006-2007Phase 1 - 2006RJB/VGMercurySeparate experiments by pulse requirements I:IFE optics testing and Phase I & II long pulseMercury URU-6-Apr-06 JD-5• Laser damage (IFE final optics) Latkowski IFE• Longevity of other IFE laser components Ebbers/Bayramian IFE• X-ray calibration (sensitivity and/or timing) Holder/Young(s)/Izumi/+ X-ray• Point projection imaging Landen X-ray• Extreme chemistry w/CARS Collins/Page Shock• X-ray diffraction of shocked materials Lorenzana/Kalantar Shock• SBS & SRS backscatter from gas/plasma Froula/Glenzer LPI• Thomson scattering (intrinsic and/or collective) Glenzer LPI• Laser-Plasma Interactions (LPI) Young/ Patel LPI• LPI – two plasmon decay (LDRD proposal) Kirkwood/Payne LPI• 1w pre-pulse effects measurements for NIF Kalantar NIF• Debris and shrapnel effects Kalantar/Koniges NIFRJB/VGMercurySeparate experiments by pulse requirements II:Short pulse Mercury, Phase IIIMercury URU-6-Apr-06 JD-6• Filamentation and remote sensing Stuart Visible light• Proton radiography MacKinnon MeV protons• Proton induced isochoric heating Patel/Eckart/Osterheld MeV protons• Fast ignitor, hot electron transport MacKinnon/Key MeV electrons• Hard x-ray backlighter development Park/Koch K-a X-rays• X-ray probe of transient lattice structure/melting Lorenzana K-a X-rays• GRIP X-ray laser and applications Dunn/Nelson/Rocca … X-ray Laser• Neutron generation for NIF sensor calibration Young Neutrons• Neutron generation for medical isotopes Ditmire Neutrons• High flux neutron source for materials research Perkins Neutrons• HEDP plasma spectroscopy development (LDRD) Shepherd/Dunn X-raysRJB/VGMercuryOur Phase I User Facility Plan will use1047 nm or frequency-doubled 524 nm beam 42 - 48”Target Chamber31”38”1047 nm524 nm60 J, 15 ns30 J, 15 ns1w absorberPeriscopeLaser diagnostic pick offDoubling crystalRJB/VGMercurySolid target inclined at an angle to divert debris and plasma blow-off from input optics F#8f = 24”Laser diagnosticsOptical Blastshield Rotating solid disk  targetSwing-inHard BlastshieldThrough imaging CCDThrough imaging opticX-ray diagnosticsRJB/VGMercuryPhase II & III:  Janus target chamber has been acquired for initial experiments on MercuryRJB/VGMercuryMercury output periscope supportØ1m target vessel8m 1:1 telescope1w, 2w final optics& beam diagnosticsWe have identified a laboratory for Phase II activities RJB/VGMercuryTwo white papers on target physics applications of Mercury have been writtenExtreme Chemistry Using Mercury—short versionRalph H. Page and Gilbert W. CollinsV Division, PAT(925) 423 6682;  L-460;  page4@llnl.gov7 Sept 05I.  IntroductionStars and giant planets contain matter that exists under ultra-high-pressure conditions,compressed several-fold with respect to its specific volume at the Earth’s surface.  At such high pressures (millions of atmospheres,) as found at the core of  the giant planets (Figure 1,) various phase changes will have occurred.  Normally-insulating materials could even exist as metals.  In this “extreme chemistry” regime, our 1-atm (1 bar) intuition no longer applies.  Starting from a “particle-in-a-box” perspective, we realize that the “boxes” have become much smaller, the energy levels have shifted, and the electronic orbitals have become distorted.  Orbital overlap, hybridization, and chemical bonding are radically different at high pressure, and although theoretical calculations have been done for many systems, stringent experimental tests are quite rare.  In fact no experiments have ever probed the chemistry or molecular bonding that might exist under such conditions.  So, we seek a means to do “extreme chemistry” experiments (at ultrahigh pressure) on Mercury, a laser system that provides the necessary and unique combination of high-energy pulses and high repetition rate enabling the signal averaging required to extract the detailed chemical nature of highly-compressed planetary fluids.Fig 1.  Matter in planets, stars, etc. exists at ultra-high pressures (over 1 million bar.)  In general, even when the chemical compositions are known, the phases are not well-established.  Jupiter and Neptune are primary examples.  Closer to home, details of Earth’s core-mantle boundary are not well-understood.II. Laser-driven shocksWhile experiments have begun to explore the pressure, density, and temperature of states expected to occur inside these giant planets, there exist no experiments looking at the high-pressure chemistry.  To get a glimpse at the chemistry governing the interiors of stars, planets, and weapons, we will create samples at high pressure and then inspect them spectroscopically.  The only way to create giant planetary core states is with 0.1 MbarH2O + CH4 + NH33 MbarH-C-N-O ices8 MbarRocks,Diamond?Mercury High Average Power X-ray LaserJames DunnInternal LLNL Report28 October 2005RJB/VGMercuryCARS probes vibrational spectrum of shocked matter; VISAR calibrates shock pressure (speed)MercuryVac. chamberw/ moving targetVISAR/streakNd:YAG Dye laserGated CCD spectrometernRnPnPnASnS nP nASI(n)Experiment proposed byRip Collins and Ralph PageRJB/VGMercuryGrazing Incidence Pumped (GRIP) x-ray laser produced by absorbing pump energy efficiently in gain region: 10 Hz XRL  (by Jim Dunn)3.02.01.00.0Counts1050-5-10Distance from target axis (mrad)2423222120191817Wavelength (nm)3210CountsR. Keenan, J. Dunn, P.K. Patel, D.F. Price, R.F. Smith, and V.N. Shlyaptsev, “High Repetition Rate Grazing Incidence Pumped X-ray Laser Operating at 18.9 nm”, Phys. Rev. Lett., 94, 103901-1 (2005).In collaboration with Slava Shlyaptsev, UC Davis•Short pulse propagates in plasma up to a specific electron density•Short pulse is then refracted back into gain region•Short pulse angle given by where ne0= density at turning point•Traveling wave pump inherent and no restriction on target length•Absorption efficiency in gain region increases to 50% for GRIPq = ne0 necExperimental Setup for 10 Hz GRIP X-ray LaserCCDSpectrometerTargetXRL7oShort pulseLong pulseOn AxisParabola14oGratingIrMirror80 mJ, 1.5 ps70 mJ, 200 psLaser Pump:150 mJ/pulse at 10 Hz18.9 nmXRL3.6 mrad08-18-05 Mercury JD-4RJB/VGMercuryHigh repetition rate target manipulator allows high average brightness x-ray laserExperimental Setup for X-ray LaserCCDSpect romet erTargetXRL7oShort pulseLong pulseOn AxisParabola14oGrat ingIrMirror• Two laser pulses required• Grazing incidence short pulse beam on target• Traveling wave achieved at close to ~cSpherical lens, f=50 cmCylindrical lens, f=400cmOn-axis parabola Ø15 cm, f =91 cmTarget DesignX-ray laser target discLine focusLaser alignment windowNumerical control stages• 40,000 shots/rotation in eroding target concept• > 1 hour/rotation at 10 Hz rate• Many rotations on 1 target discR. van MarenX-ray laserRJB/VGMercuryHigh average spectral brightness soft x-ray (60 to 200 eV) sources can be achieved on MercuryAverage Spectral Brightness vs E for Present and Future X-ray SourcesPresentGRIPProjected GRIP 13.9 nm (89 eV) XRL pumped by 1 J, 30 Hz laser drivePresent GRIP 18.9 nm (66 eV) XRL pumped by 0.15 J, 10 Hz Callisto driveMercuryRJB/VGMercuryNew concepts are being developed for rapid target insertion and manipulationTarget ChamberTargets on conveyor beltSupply Reel Take-up ReelFocus Lens PortSeveral complex target shots per second are possible with such a systemRJB/VGMercurySummary• Mercury User facility is highly synergistic with IFE goals• We seek missions within NNSA that will result in new, unique capabilities, based on high rep rate.• Several potential applications that have been proposed.– Short pulse applications appear most interesting – Short pulse laser architecture based on Ti:Sapphire likely due to long pulse duration of Mercury in near term• Target manipulation and target debris are major issues to be addressed.• Preliminary layout of target facility has been developed• Draft schedule:– Phase I 2006, Mercury laboratory– Phase II 2007, new laboratory and target chamber– Phase III 2007- 2009, short pulse added

Mercury: A High Repetition Rate Laser for High Energy Density Physics

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Mercury: A High Repetition Rate Laser for High Energy Density Physics

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