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Rochester - OPT - 253
Lab 2: Single Photon InterferenceRoger A. Smith OPT 253 The Institute of Optics University of Rochester Rochester, NY 14627 December 5, 2008Abstract The purpose of this experiment was to explore the eects of wave-particle duality that cause photons
Rochester - OPT - 253
Lab 3-4: Single Photon SourceRoger A. Smith OPT 253 Lukishova The Institute of Optics University of Rochester Rochester, NY 14627 December 5, 2008Abstract With the advent of the novel applications of quantum mechanics, reliable single photon source
Rochester - OPT - 253
Lab 1 ReportCarlin GettliffeAbstract: In this lab we produced entangled photon pairs and used avalanche photo diodes to record coincidence counts in order to confirm a violation of Bells inequality. The entangled photons were produced by spontane
Rochester - OPT - 253
September 30, 2008 Submitted for the partial fullment of the course PHY 434Single Photon Sources and Their ApplicationsMayukh Lahiri1, 1Department of Physics and Astronomy,University of Rochester, Rochester, NY 14627, U.S.AElectronic addr
Rochester - OPT - 253
Carlin Gettliffe OPT 253 09/27/08Single Photon Sources and Their ApplicationsThe primary application for single photon production is in quantum computing. The ability to reliably produce single photons could eventually lead to efficient and highl
Rochester - OPT - 253
Lab 3/4 Report Carlin GettliffeAbstract: In this lab we investigated the quantum dot excitation method of single photon production. Objectives included preparing quantum dot samples in a liquid crystal solution, successfully imaging fluorescence em
Rochester - FIW - 06
Impact Fast Ignition Another Pathway to IgnitionImpactor Main FuelFast Ignition Workshop 06 4 November 2006 Cambridge, MAH. Azechi et al. Institute of Laser Engineering Osaka University1CollaboratorsILE OSAKAInstitute of Laser Engineering
Rochester - FIW - 06
Recent developments in proton acceleration, beam handling, and applications in plasma physicsJulien FuchsFI workshop Cambridge, MALABORATOIRE POUR L'UTILISATION DES LASERS INTENSESOutlineI. Prospects in proton energy increase using very thin ta
Rochester - FIW - 06
Fast Ignition Integrated Simulation for FIREX-I ProjectT.Johzaki Institute of Laser Engineering, Osaka University In collaboration with S. Sakagami*, H. Nagatomo, T. Nakamura, K. Mima, Y. Nakao*, FI3 project team and FIREX project teamInstitute of
Rochester - FIW - 06
National Ignition Facility Status and Plans and Fast Ignition CapabilitiesPresentation to 9th International Fast Ignition Workshop Cambridge, MADr. Edward I. Moses Associate Director National Ignition Facility Programs Lawrence Livermore National
Rochester - FIW - 06
FSCGain Curves for Fast-Ignition Inertial Confinement FusionEFusion GM = EDriver EFusion GT = EDriver + EPetawattA. A. Solodov, R. Betti, J. A. Delettrez, and C. Zhou Fusion Science Center Laboratory for Laser Energetics University of Rochester
Rochester - FIW - 06
LA-UR-06-7585Theory and Modeling of LaserAccelerated Ion Beams as Possible Fast IgnitorsBrian J. Albright, Lin Yin, B. Manuel Hegelich, Kevin J. Bowers*, Kirk A. Flippo, Thomas J. T. Kwan, and Juan C. Fernndez Los Alamos National Laboratory9th In
Rochester - FIW - 06
Integrated Modeling of Fast Ignition ExperimentsPresented to: 9th International Fast Ignition Workshop Cambridge, MA November 3-5, 2006R. P. J. Town AX-Division Lawrence Livermore National LaboratoryThis work was performed under the auspices of
Rochester - FIW - 06
Direct-drive targets for fast ignition: design issues and options on the path to high gainS. Atzeni1, C. Bellei1,2 and A. Schiavi11) Dipartimento di Energetica, Universit di Roma La Sapienza,Italy 2) Blackett Laboratory, Imperial College, Prince Co
Rochester - FIW - 06
FSCFast-Ignition Research at the Laboratory for Laser EnergeticsHot-electron generation and heating Fuel assemblyabn tW. Theobald University of Rochester Laboratory for Laser Energetics9th International Fast Ignition Workshop Cambridge,
Rochester - FIW - 06
Diagnostics for Fast-Ignitor Experiments on OMEGA/OMEGA EPMTW target chamber 9th International Fast Ignition Workshop Cambridge, MA 35 November 2006C. Stoeckl University of Rochester Laboratory for Laser EnergeticsSummaryDiagnostic developmen
Rochester - FIW - 06
Design of a Pair-Plasma Production Experiment for OMEGA EPccJ. Myatt, A. V. Maximov, and R. W. Short University of Rochester Laboratory for Laser Energetics9th International Fast Ignition Workshop Cambridge, MA 35 November 2006SummaryOMEG
Rochester - FIW - 06
Short pulse laser driven relativistic electron transport in wire targetsR. J. Mason*, R. B. Stephens1, M. Wei2, R. R. Freeman3, J. Hill3, L. D. Van Woerkom3 1General Atomics, 2UCSD, 3The Ohio State Univ. *Research Applications Corp. 9th Internationa
Rochester - FIW - 06
HiPER: a laser fusion facility for EuropeProf Mike DunneDirector, Central Laser Facility, Rutherford Appleton Laboratory, UKm.dunne@rl.ac.ukwww.hiper-laser.euWe are entering a new era Demonstration of IFE ignition within ~ 5 years Visibilit
Rochester - FIW - 06
Full scale PIC simulation of cone-guided fast ignitionYasuhiko Sentoku A. Kemp*, B. Chrisman, and T. Cowan University of Nevada, Reno *Lawrence Livermore National Laboratory 11/05/2006@Boston9th International Fast Ignition WorkshopFast Ignition-
Rochester - FIW - 06
Hydrodynamic Simulations of Integrated Fast-Ignition Experiments Planned for OMEGA/OMEGA EP Laser SystemsnnnJ. A. Delettrez University of Rochester Laboratory for Laser Energetics9th International Fast Ignition Workshop Cambridge, MA 35 Nov
Rochester - FIW - 06
Preperations for Integrated Cryogenic Fast-Ignition Experiments on OMEGA/OMEGA EPb-layered DT Cryogenic TargetOMEGA EPDavid D. Meyerhofer Director, Experimental Division Laboratory for Laser Energetics ME and Physics Departments University of R
Rochester - FIW - 06
Collisional Relaxation of Super Thermal Electrons Generated by Relativistic Laser Pulses in Dense PlasmaPresented to: APS-DPP PhiladelphiaAndreas J. Kemp(1) Y. Sentoku(2), V.Sotnikov (2) and S.C.Wilks(1)(1)Lawrence Livermore National Laborator
Rochester - FIW - 06
Fast electron transport and heating induced by ultra-intense laser beamP.Guillou1, P.Audebert1, C.Back2, B.Barbrel1, S.Bastiani-Ceccotti1, S.D.Baton1, C.Blancard3, E.Gauci1, L.Gremillet3, M.Koenig1, L. Lecherbourg1, C.Rousseaux3, T.Vinci11Laboratoi
Rochester - FIW - 06
Proton acceleration from critical density foams with the Vulcan Petawatt laserL Willingale1, SPD Mangles1, SR Nagel1, C Bellei1, RJ Clarke2, AE Dangor1, R Heathcote2, N Lopes3, M Kaluza1, C Kamperidis1, S Kneip1, K Marsh4, Z Najmudin1, W Nazarov5, P
Rochester - FIW - 06
Physics of ion beam pulse neutralization by background plasmaOutlineWhy volumetric plasma has to be used for intense ion beam focusing. Key plasma parameters for good charge and current neutralization in a background plasma.I.D. Kaganovich, A. B
Rochester - FIW - 06
Integrated 1D PIC Simulation of Fast IgnitionBrian Chrisman Y. Sentoku A. Kemp T. E. Cowan University of Nevada, Reno1D PIC Simulations provide insight into fast ignition physicsImportant physics in FIHot electron and fast ion generation Energy
Rochester - FIW - 06
Kinetic Simulations of UltraFast Laser-Induced Fusion in Overdense TargetsP. Messmer*, K. Paul, W.L.Wang, P. StoltzTech-X Corporation AFRL Edwards Air Force Base Work supported by DoD SBIR Grant #FA8650-04-C-2511*email: messmer@txcorp.comJ.-L. C
Rochester - FIW - 06
SummaryPreliminary cone-in-shell simulations agree well with experimentFSC 2-D cone-in-shell fuel-assembly simulations are being simulated using HYDRA* Simulated tRs and convergence ratios are in agreement with experiment*M. M. Marinak et al.
Rochester - FIW - 06
A Novel Method for Using an Arbitrary EOS in PIC Simulations of Laser-Target Interactions*W. M. Sharp, D. P. Grote, M. Tabak, B. C. McCandless, and A. J. Kemp LLNL9th International Fast Ignition Workshop Cambridge, MA 4 November 2006*This work wa
Rochester - FIW - 06
Optical Probing of Underdense LaserPlasma Interactions Using the Vulcan Petawatt LaserImperial College LondonP. M. Nilson University of Rochester Laboratory for Laser Energetics9th International Workshop on Fast Ignition Targets Cambridge, MA 3
Rochester - FIW - 06
FSCFast-Ignition Fuel Assembly: Theory and Experimentst D t tt DC. Zhou and R. Betti University of Rochester Laboratory for Laser Energetics9th International Fast Ignition Workshop Cambridge, MA 35 November 2006SummaryScaling laws for f
Rochester - FIW - 06
High-Intensity Laser Interactions with Solid Targets and Implications for Fast-Ignition Experiments on OMEGA EPannnnnJ. Myatt University of Rochester Laboratory for Laser Energetics48th Annual Meeting of the American Physical Society D
Rochester - FIW - 06
X-ray and Proton Generation at the 40TW-Level with Z-Petawatt9th International Fast Ignition WorkshopCambridge, November 3, 2006 Matthias Geissel, B.W. Atherton, E. Brambrink, A.D. Edens, P.K. Rambo, and J. Schwarz Sandia National LaboratoriesSNL
Rochester - FIW - 06
Quasi-DC Probing of Electrical Conductivity in Warm Dense Matter Quasi-DC Probing of Electrical Conductivity in Warm Dense MatterG. Rodriguez, K. Y. Kim, B. Yellampalle, A. J. Taylor, and J. H. Glownia Los Alamos National Laboratory, Los Alamos, NM
Rochester - AST - 142
Useful formulasEnergy, luminosity, flux L = dE dt f = L 4 r 2df = B (T ) d df = T4L = 4 R 2 T 4maxT = 0.29 cm KEnergy density and pressure of radiation: ur = 4 4 T 4 f = c c dE dt P = nkT = kT m Pradiation = 4 T 4 3cRest energy: E = m0 c
Rochester - AST - 111
The Revolution of the Moons of JupiterStudent ManualA Manual to Accompany Software for the Introductory Astronomy Lab Exercise Document SM 1: Version 1Department of Physics Gettysburg College Gettysburg, PA 17325 Telephone: (717) 337-6028 email:
Rochester - AST - 111
Astronomy 111 Lab ManualFall 2003What is expected in a Lab reportYour lab report doesnt need to be very long or detailed. However, it needs to reflect an understanding of what the experiment was for, it needs a description in legible form of the
Rochester - AST - 111
The Celestial GlobeOriginally based on: http:/pegasus.phast.umass.edu/a100/handouts/celest.html http:/astrosun.tn.cornell.edu/courses/astro201/cel_sphere.htmAstronomers view the sky (half-hemisphere) available to us above the horizon at any time,
Rochester - AST - 111
Astronomy 111 Lab ManualFall 2004Scattering and Extinction of Light by Small Particles 1. Introduction1.1 Absorption and ScatteringIf we understand how light passes through planetary atmospheres we can learn about these planetary atmospheres fr
Rochester - A - 241
Handout 12: Limb darkening, absorption linesWhen v = 2/3T = effective temperatureWe "see" to = 1 at each This corresponds to v < 1 Average over all gives <v> = 2/3With the source function, we can calculate limb darkening 2 3 3 4 4 ( ) 2S
Rochester - AST - 111
Astronomy 111 ManualFall 2004Lab: Rotation period of the sun from sunspotsIntroductionThe Sun rotates about an axis inclined by about 7 with respect to the axis of the solar system (the axis perpendicular to the ecliptic). The easiest way to se
Rochester - A - 241
Handout 11: Solutions to equation of Radiative TransferConsider the case where the source function S is constant in spacei.e. T.E. and T = const.First approximation- - + S 1 - e SolutionIf S = 0,I ( )I ( 0) emerely extinction, I
Rochester - A - 453
Lecture 28 Radiation Pressure Too date, we have ignored radiation pressure adequate for solar-mass main sequence stars The disagreement of the grey atmosphere with the Kurucz accurate 50,000 K models can largely be attributed to this neglect Rad
Rochester - A - 453
Lecture 18: Solution of Equation of Radiative Transfer The equation looks fairly simple dI = (j - I )ds If we knew the state of matter, we should be able to calculate j and and solve this. Problem: to know state of matter (i.e. ionization, ex
Rochester - A - 453
Lecture 20 2nd Moment Equation of Transfer Multiply both sides of the equation of transfer by cos() and integrate over the unit sphere. dI 2 cos ( ) = cos( ) ( I S ) d 4 sterdagain d d but and and sod cos 2 ( ) = 0 so: d2 4 44 I
Rochester - A - 453
Lecture 24: Absorption lines in real stellar atmosphere The reversing layer model used to date was a convenient approximation Gives main features of real lines Line shape gaussian for weak lines Thermal doppler plus turbulent doppler give gaussia
Rochester - A - 241
Handout 19: Evolution of stars on the Hertzsprung-Russell DiagramFrom H.W. #7:Adiabatic T gradient is : cP cV so dln( T) dln( P) dln( T) dln( P) 1 cP cV cPIf the T-gradient required by radn xfer in order to transport the L outward is steeper t
Rochester - A - 241
Handout 20: Evolution and Nature of starsTo recapLow T stars are fully convectiveHigh Kramers opacity in the interior High heat capacity just below the photosphereH and He ionizationLuminosity determined by matching convective interior to radia
Rochester - A - 453
Uniform stellar model M := M sun R := Rsun := M ( r) := 4 3 r 3 := 0.62 M constant, the "water sun" 4 R3 3 G M ( r) dr P( r) = P( R) 2 r R 2rhydrostatic equilibriumP( r) :=2 3 G R r9(22)set P(R) = 0P( 0
Rochester - A - 241
Handout 15: Virial Theorem E = P.E. + K.E = (1/2)P.E. = -K.E.The virial theorem is crucial for an overview of the stellar interiorSee discussion Chap. 2 of C&OHolds when P.E. is from a force ~ 1/r2i.e. gravity and electrostatic forcesConsider
Rochester - A - 453
Atomic absorption cross sections =2 e_2me cf= f ( ) f-value, line strength.line shape has property ( ) d = 1 0 FWHM = c 02hence 0 =( )1 FWHMapproximately, and FWHM2 e_2so, at line center 0 f , , 0 := f
Rochester - A - 241
Handout 3: Chap. 5: Light & MatterIf everything radiated like a blackbody, spectra would be quite boring. In fact, deviations from a blackbody tell us a lot about stars (and the rest of the universe). Deviations occur for many reasons. Some objects
Rochester - A - 241
Handout 23: Star FormationReview collapse of a starConditions for collapse (Jeans)If gravity > thermal pressure collapsei.e. not hydrostatic equilibriumFor a given cloud with (,T)M > MJeans ~ T3/2-1/2 Or R > RJeans ~ T1/2-1/2Note: such regi
Rochester - A - 241
Handout 7 Chap. 9 Stellar AtmospheresGoalsUnderstand why stellar spectra closely resemble black bodiesi.e. shape of F vs ~ B(Te) L = 4r2Te4Deviations from a blackbodyi.e. absorption linesGive Temperature Give abundances of nCa/nH, etc. Give L
Rochester - SCIENCEV - 323
Rochester - A - 241
Handout 9: Radiative transfer in a starSince Intensity is conserved in free space, we need only deal with interaction of light with matterTo properly account for these interactionsWe need the density of matter Also, the compositioni.e. H:He:C:N:O
Rochester - A - 453
Lectures 2-3 notes 1 2 g t = h 2 2 10 kmg := free-fall time at const. accel=45.16 secg=980.66 cmsec-3-2Msun4 3 Rsun 3 1= = 1.39 gmcmaverage solar densityG 54.7 min23 1 = 0.49 hr 32 G free-fall time scale7 1
Rochester - SCIENCEV - 323
Rochester - A - 453
More realistic line profiles, using Eddington Approximation for T structure Te :=5800 K4model the solar spectrumT ( ) := Te 3 2 + 4 3Eddington Approximation for T structure1.5 .104T(0) = 4877 KT 2 = 5800 K 3T 0 i( )
Rochester - A - 241
Nature of LightTwo aspects both importantWaveYoungs double slit destructive and constructive interference of monochromatic light. i.e.If (path length) = n, constructive If (path length) = (n+1/2), destructive Where = c, fundamental constantM