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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
Rochester - A - 241
Handout 16: Nature of a StarR/Rsun 10 5 2 1 <T> 106 K 2 106 K 5 106 K 107 K t tK-H ~ 104 y tK-H ~ 105 y tK-H ~ 106 y Nucl. Reactions start Nucl. Reactions dominatetnucl ~ 1010 y Main SequenceThe contraction stops when d(Enucl)/dt in the interior
Rochester - A - 453
0 :=656.3 nm := 20.04 nm 0 :=.2Balmer alpha line , 0 := 0 e () 0 Gaussian profile continuum flux 0 proportional to column densityFc :=1FF , ,2 0 := Fc e i i :=( ) ) , 0()reversing layer model f
Rochester - A - 241
Handout 6 Chap. 8 Spectral ClassificationClass based on strength of absorption lines in spectrum (see v.g.)T increasing O B A F G K M H lines Ca II TiO molecules weak S weak weak S S weakweak S, strongVisible (Balmer) H linesArise from n=2 lev
Rochester - SCIENCEV - 323
Rochester - AST - 111
Astronomy 111 Lab ManualFall 2004LAB #8The Solar wind and the Earths magnetosphereI. Introduction Geomagnetic storms are a natural hazard, like hurricanes and tsunamis, which the National Oceanic and Atmospheric Administration (NOAA) Space Env
Rochester - AST - 142
Physical and astronomical constantsGravitational constant Boltzmann constant Stefan-Boltzmann constant Planck constant Speed of light Electron mass Proton mass Neutron mass Hydrogen mass Atomic mass unit Quantum of electric charge, cgs Quantum of el
Rochester - AST - 111
AST111 Lecture 4aTelescopes4m Mayall telescope of NOAO on Kitt PeakWhat a Telescope does Light gathering power, so we can see fainter objects. Telescopes can also be made to gather light at wavelengths that we can't see with our eyes. Provide
Rochester - AST - 111
Problem Set #1, AST111 Solutions1) Sidereal and solar periods. See PS (Planetary Sciences) problems 1.3-1.5. A planet which keeps the same hemisphere pointed toward the Sun must rotate once per orbit in the prograde direction (i.e., in the same rota
Rochester - AST - 142
Astronomy 142 Midterm Exam #1Thursday March 20, 2008 11:05AM-12:20PM, B+L407Exam rules: you may consult only one page of formulas and constants and a calculator while taking this test. You may not consult any books, nor each other. All of your wor
Rochester - AST - 111
Problem Set #1, AST111due Tuesday Sept 14, beginning of class1) Sidereal and solar periods. See PS (Planetary Sciences) problems 1.3-1.5. A planet which keeps the same hemisphere pointed toward the Sun must rotate once per orbit in the prograde di
Rochester - AST - 111
Problem Set #5, AST111Solutions 1) Calculate the equilibrium temperature of the Moon as a function of latitude. Assume that the moon is a rapid rotator with zero obliquity, has a bond albedo of Ab=0.07 and an emissivity of 1.For a small ribbon of
Rochester - AST - 142
Astronomy 142 Midterm Exam #1 SolutionsShort Problems (Choose 4 of 6 parts) In the absence of extinction an O5 star has colors U-B =-1.1 and B-V=-0.3. Its absolute magnitude is MV =-5.6. Interstellar extinction has extinction ratio A(B)/A(V) = 1.34
Rochester - AST - 111
Problem Set #7, AST111 Solutions1) The Voyager 1 spacecraft detected nine active volcanoes on Io. Assume that, on average, there are nine volcanoes active on Io, and that the average eruptive rate per volcano is 50km3/yr. The radius of Io is 1820 km
Rochester - AST - 111
Astronomy 111 Lab ManualFall 2004Scaling of Splash Craters and Ejecta TrajectoriesIntroductionThe surface of many bodies in our solar system exhibit evidence for impact craters. Some surfaces, like portions of the Moon appear saturated with cra
Rochester - AST - 111
Overview of the Solar systemThis is a composite image of all the planets in our solar system. From the top is Mercury (taken by the Mariner 10 spacecraft); Venus (taken by the Pioneer Venus Orbiter); a full disk of the Earth (taken by the Apollo 17
Rochester - AST - 142
Today in Astronomy 142: the Milky Way, continuedStellar relaxation time Virial theorem Differential rotation of the stars in the disk The local standard of rest Rotation curves and the distribution of mass The rotation curve of the GalaxyFigure: sp
Rochester - AST - 111
Problem Set #5, AST111due Tuesday Oct 12, beginning of class 1) Calculate the equilibrium temperature of the Moon as a function of latitude (see PS problems 3.5, 3.6). Assume that the moon is a rapid rotator with zero obliquity, has a bond albedo of
Rochester - AST - 111
AST111, Lecture 1bPlanetary properties (overview continued) The Celestial Sphere (our coordinate system).Planetary properties (continued): Measuring Mass The orbital period of a moon about a planet depends on the semi-major axis and on the plane
Rochester - PHY - 103
Student projects for PHY103 (2008)The physics of/and music encompasses a wide range of topics, some that we will cover in labs and lectures in this class. However the diversity of subject matter related to this topic cannot be captured in a single s
Rochester - AST - 111
AST111 - Elementary Astronomy: Origins of the Solar System and BeyondLectures: TR 11:05am -12:20pm, Bausch and Lomb Hall (B+L) Room 270 Workshops: M7-9pm, B+L480, by tradition. Problem sets are due the next day at the beginning of class. Labs: R 6:
Rochester - AST - 111
Problem Set #4, AST111Solutions 1) On Spectral resolution and Absolute magnitude. When you observe with your eye you see light over a large wavelength range (about 4000-7000). We can think of the eye as having spectral resolution R ~ 5. Supposing yo
Rochester - AST - 111
Relected light from dust in AB Aurigas debris diskAST111, Lecture 3bAST111, Lecture 3bThe Dynamics of Small Bodies Dissipative and Radiation ForcesAdditional Forces on Small BodiesFor planets, gravity is the largest force. However small bodi