Topical Review: Relativistic Laser-Plasma Interactions
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High Energy Density Physics Experiments at Los Alamos
High Energy Density Dante-2 SXI Physics Experiments at Los Alamos FFLEX FABS & Hans Herrmann NBI FABS & 36B NBI 31B Dante-1 Plasma Physics Group (P-24) SXI In this photo, Norris Bradbury, Robert Oppenheimer, Richard Feynman, and Enrico Fermi attend an early Los Alamos weapons colloquium. OMEGA LaserU UserN C L A S SGroup I F I E D Rochester, NY April 29, 2011 Operated by Los Alamos National Security, LLC for NNSA LA-UR 11-02522 Los Alamos has a strong program in High Energy Density Physics aimed at National Applications as well as Basic Science Inertial Confinement Fusion (ICF) Radiation Hydrodynamics Hydrodynamics with Plasmas Material Dynamics Energetic Ion generation Dense Plasma Properties X-ray and Nuclear Diagnostic Development Petaflop performance to Exascale computing Magnetic Reconnection Magnetized Target Fusion High-Explosive Pulsed Power U N C L A S S I F I E D Operated by Los Alamos National Security, LLC for NNSA LANL is a multidisciplinary NNSA Lab. overseen by Los Alamos National Security (LANS) LLC. People 11,782 total employees: LANS, LLC 9,665; SOC Los Alamos (Guard Force) 477; Contractors 524; Students 1,116 Place Located 35 miles northwest of Santa Fe, New Mexico, on 36 square miles of DOE-owned property. > 2,000 individual facilities, 47 technical areas with 8 million square feet under roof, $5.9 B replacement value. Operating costs FY 2010: ~ $2 billion 51% NNSA weapons programs 8% Nonproliferation programs 6% Safeguards and Security 11% Environmental Management 4% DOE Office of Science 5% Energy and other programs 15% Work for Others Workforce Demographics (LANS & students only) 42% of employees live in Los Alamos, the rest commute from Santa Fe, Española, Taos, and Albuquerque. -
The National Ignition Facility Diagnostic Set at the Completion of the National Ignition Campaign, September 2012
Fusion Science and Technology ISSN: 1536-1055 (Print) 1943-7641 (Online) Journal homepage: http://www.tandfonline.com/loi/ufst20 The National Ignition Facility Diagnostic Set at the Completion of the National Ignition Campaign, September 2012 J. D. Kilkenny, P. M. Bell, D. K. Bradley, D. L. Bleuel, J. A. Caggiano, E. L. Dewald, W. W. Hsing, D. H. Kalantar, R. L. Kauffman, D. J. Larson, J. D. Moody, D. H. Schneider, M. B. Schneider, D. A. Shaughnessy, R. T. Shelton, W. Stoeffl, K. Widmann, C. B. Yeamans, S. H. Batha, G. P. Grim, H. W. Herrmann, F. E. Merrill, R. J. Leeper, J. A. Oertel, T. C. Sangster, D. H. Edgell, M. Hohenberger, V. Yu. Glebov, S. P. Regan, J. A. Frenje, M. Gatu-Johnson, R. D. Petrasso, H. G. Rinderknecht, A. B. Zylstra, G. W. Cooper & C. Ruizf To cite this article: J. D. Kilkenny, P. M. Bell, D. K. Bradley, D. L. Bleuel, J. A. Caggiano, E. L. Dewald, W. W. Hsing, D. H. Kalantar, R. L. Kauffman, D. J. Larson, J. D. Moody, D. H. Schneider, M. B. Schneider, D. A. Shaughnessy, R. T. Shelton, W. Stoeffl, K. Widmann, C. B. Yeamans, S. H. Batha, G. P. Grim, H. W. Herrmann, F. E. Merrill, R. J. Leeper, J. A. Oertel, T. C. Sangster, D. H. Edgell, M. Hohenberger, V. Yu. Glebov, S. P. Regan, J. A. Frenje, M. Gatu-Johnson, R. D. Petrasso, H. G. Rinderknecht, A. B. Zylstra, G. W. Cooper & C. Ruizf (2016) The National Ignition Facility Diagnostic Set at the Completion of the National Ignition Campaign, September 2012, Fusion Science and Technology, 69:1, 420-451, DOI: 10.13182/FST15-173 To link to this article: http://dx.doi.org/10.13182/FST15-173 Published online: 23 Mar 2017. -
Chapter 3 the Mechanisms of Electromagnetic Emissions
BASICS OF RADIO ASTRONOMY Chapter 3 The Mechanisms of Electromagnetic Emissions Objectives: Upon completion of this chapter, you will be able to describe the difference between thermal and non-thermal radiation and give some examples of each. You will be able to distinguish between thermal and non-thermal radiation curves. You will be able to describe the significance of the 21-cm hydrogen line in radio astronomy. If the material in this chapter is unfamiliar to you, do not be discouraged if you don’t understand everything the first time through. Some of these concepts are a little complicated and few non- scientists have much awareness of them. However, having some familiarity with them will make your radio astronomy activities much more interesting and meaningful. What causes electromagnetic radiation to be emitted at different frequencies? Fortunately for us, these frequency differences, along with a few other properties we can observe, give us a lot of information about the source of the radiation, as well as the media through which it has traveled. Electromagnetic radiation is produced by either thermal mechanisms or non-thermal mechanisms. Examples of thermal radiation include • Continuous spectrum emissions related to the temperature of the object or material. • Specific frequency emissions from neutral hydrogen and other atoms and mol- ecules. Examples of non-thermal mechanisms include • Emissions due to synchrotron radiation. • Amplified emissions due to astrophysical masers. Thermal Radiation Did you know that any object that contains any heat energy at all emits radiation? When you’re camping, if you put a large rock in your campfire for a while, then pull it out, the rock will emit the energy it has absorbed as radiation, which you can feel as heat if you hold your hand a few inches away. -
Analysis of the Cyclotron Radiation from Relativistic Electrons Interacting with a Radio-Frequency Electromagnetic Wave
Progress In Electromagnetics Research B, Vol. 52, 117{137, 2013 ANALYSIS OF THE CYCLOTRON RADIATION FROM RELATIVISTIC ELECTRONS INTERACTING WITH A RADIO-FREQUENCY ELECTROMAGNETIC WAVE Christos Tsironis* Department of Physics, Aristotle University of Thessaloniki, Thessa- loniki 54 124, Greece Abstract|The emission of electromagnetic radiation from charged particles spiraling around magnetic ¯elds is an important e®ect in astrophysical and laboratory plasmas. In theoretical modeling, issues still not fully resolved are, among others, the inclusion of the recoil force on the relativistic electron motion and the detailed computation of the radiation power spectrum. In this paper, the cyclotron radiation emitted during the nonlinear interaction of relativistic electrons with a plane electromagnetic wave in a uniform magnetic ¯eld is examined, by analyzing the radiated power in both time and frequency domain. The dynamics of the instantaneous radiation and the emitted power spectrum from one particle, as well as from monoenergetic electron ensembles (towards a picture of the radiation properties independent of the initial conditions) is thoroughly studied. The analysis is performed for several values of the wave amplitude, focusing near the threshold for the onset of nonlinear chaos, in order to determine the alteration of the radiation in the transition from regular to chaotic motion. 1. INTRODUCTION An important factor in systems involving charged particle acceleration by electromagnetic waves, especially for diagnostic measurements, is the -
Plasma Interactions
Home Search Collections Journals About Contact us My IOPscience New developments in energy transfer and transport studies in relativistic laser–plasma interactions This article has been downloaded from IOPscience. Please scroll down to see the full text article. 2010 Plasma Phys. Control. Fusion 52 124046 (http://iopscience.iop.org/0741-3335/52/12/124046) View the table of contents for this issue, or go to the journal homepage for more Download details: IP Address: 130.183.90.175 The article was downloaded on 04/01/2011 at 10:43 Please note that terms and conditions apply. IOP PUBLISHING PLASMA PHYSICS AND CONTROLLED FUSION Plasma Phys. Control. Fusion 52 (2010) 124046 (7pp) doi:10.1088/0741-3335/52/12/124046 New developments in energy transfer and transport studies in relativistic laser–plasma interactions P A Norreys1,2,JSGreen1, K L Lancaster1,APLRobinson1, R H H Scott1,2, F Perez3, H-P Schlenvoight3, S Baton3, S Hulin4, B Vauzour4, J J Santos4, D J Adams5, K Markey5, B Ramakrishna5, M Zepf5, M N Quinn6,XHYuan6, P McKenna6, J Schreiber2,7, J R Davies8, D P Higginson9,10, F N Beg9, C Chen10,TMa10 and P Patel10 1 Central Laser Facility, STFC Rutherford Appleton Laboratory, Harwell Science and Innovation Campus, Didcot, Oxon OX11 0QX, UK 2 Blackett Laboratory, Imperial College London, Prince Consort Road, London SW7 2BZ, UK 3 Laboratoire pour l’Utilisation des Lasers Intenses, Ecole´ Polytechnique, route de Saclay, 91128 Palaiseau Cedex, France 4 Centre Lasers Intenses et Applications, Universite´ Bordeaux 1-CNRS-CEA, Talence, France 5 School of Mathematics and Physics, Queens University Belfast, Belfast BT7 1NN, UK 6 Departmnet of Physics, University of Strathclyde, John Anderson Building, 107 Rottenrow, Glasgow G4 0NG, UK 7 Max-Planck-Institut fur¨ Quantenoptik, Hans-Kopfermann-Str. -
B O O K O F a B Stra C Ts
Book of Abstracts Program Tuesday, June 25 11:00-13:00 Registration 12:00-13:50 Lunch 13:50-14:00 Welcome UHI 1 Chair : L. Yin 14:00-14:30 A. Kemp Kinetic particle-in-cell modeling of Petawatt laser plasma interaction relevant to HEDLP experiments 14:30-14:50 R. Shah Dynamics and Application of Relativistic Transparency 14:50-15:10 C. Ridgers QED effects at UI laser intensities 15:10-15:30 L. Cao Efficient Laser Absorption, Enhanced Electron Yields and Collimated Fast Electrons by the Nanolayered Structured Targets 15:30-16:00 Coffee break Laboratory Astrophysics 1 Chair : P. Drake 16:00-16:30 J. Bailey Laboratory opacity measurements at conditions approaching stellar interiors 16:30-16:50 A. Pak Radiative shock waves produced from implosion experiments at the National Ignition Facility 16:50-17:10 B. Albertazzi Modeling in the Laboratory Magnetized Astrophysical Jets: Simulations and Experiments 17:10-17:30 C. Kuranz Magnetized Plasma Flow Experiments at High-Energy-Density Facilities Wednesday, June 26 ( Joint with WDM ) ICF 1 Chair : A. Casner 09:00-09:40 N. Landen Status of the ignition campaign at the NIF 09:40-10:00 G. Huser Equation of state and mean ionization of Ge-doped CH ablator materials 10:00-10:20 B. Remington Hydrodynamic instabilities and mix in the ignition campaign on NIF: predictions, observations, and a path forward 10:20-10:40 M. Olazabal Laser imprint reduction using underdense foams and its consequences on the hydrodynamic instability growth 10:40-11:10 Coffee break XFEL Chair : B. -
Book of Abstracts
First LMJ-PETAL User Meeting October 4-5, 2018 Le Barp, France Book of Abstracts Program LMJ-PETAL User Meeting Thursday 4 October 2018 Schedule Duration Title Speaker Institution 8:00 AM 0:30 Accueil ILP 8:30 AM 0:30 Welcome Plenary session-1 : LMJ-PETAL performance Chairman : JL. Miquel CEA/DAM CEA/DAM, 9:00 AM 0:25 LMJ Facility: Status and Performance P. Delmas France CEA/DAM, 9:25 AM 0:25 PETAL laser performance N. Blanchot France CEA/DAM, 9:50 AM 0:25 Status on LMJ-PETAL plasma diagnostics R. Wrobel France Preliminary results from the qualification experiments of the PETAL+ 10:15 AM 0:25 D. Batani CELIA, France diagnostics 10:40 AM 0:20 Break Plenary session-2: Next user experiments Chairman : D. Batani CELIA Effect of hot electrons on strong shock generation in the context of shock 11:00 AM 0:25 S. Baton LULI, France ignition 11:25 AM 0:25 Investigating magnetic reconnection in ICF conditions S. Bolanos LULI, France Efficient Creation of High-Energy-Density-State with Laser-Produced Strong S. Fujioka ILE, Osaka U., 11:50 AM 0:25 Magnetic Field or K. Matsuo Japan 12:15 PM 2:00 Lunch / Posters session 2:15 PM 1:30 Round table -1 Targets Chairman: M. Manuel General Atomic CEA/DAM, 0:20 Target laboratory on LMJ Facility O. Henry France Review of General Atomics Target Fabrication : Facilities, Capabilities and General Atomic, 0:20 M. Manuel Notable Recent Developments USA Diagnostics Chairman: W.Theobald LLE Omega ILE, Osaka U., 0:20 Visualization of fast heated plasma by X-ray fresnel phase zone plate K. -
The X-Ray Imaging Polarimetry Explorer
Call for a Medium-size mission opportunity in ESA‟s Science Programme for a launch in 2025 (M4) XXIIPPEE The X-ray Imaging Polarimetry Explorer Lead Proposer: Paolo Soffitta (INAF-IAPS, Italy) Contents 1. Executive summary ................................................................................................................................................ 3 2. Science case ........................................................................................................................................................... 5 3. Scientific requirements ........................................................................................................................................ 15 4. Proposed scientific instruments............................................................................................................................ 20 5. Proposed mission configuration and profile ........................................................................................................ 35 6. Management scheme ............................................................................................................................................ 45 7. Costing ................................................................................................................................................................. 50 8. Annex ................................................................................................................................................................... 52 Page 1 XIPE is proposed -
Eyes for Gamma Rays” Though the Major Peaks Suggest a Periodic- Whether These Are Truly Gamma-Ray Bursts for a Description of This System)
sion of regularity and slow evolution in the They suggested that examination of the Vela exe-atmospheric nuclear detonation. Surpris- universe persisted into the 1960s. data might disclose evidence of bursts of ingly, however, the survey soon revealed that The feeling that transient cosmic events gamma rays at times close to the appearance the gamma-ray instruments on widely sepa- were rare was certainly prevalent in 1959 of supernovae. Such searches were con- rated satellites had sometimes responded when summit meetings were being held be- ducted; however, no distinctive signals were almost identically. Some of these events were tween England, the United States, and found. attributable to solar flare activity. However, Russia to discuss a nuclear test-ban treaty. On the other hand, there was evidence of one particularly distinctive event was dis- One key issue was the ability to detect treaty variability that had been ignored. For exam- covered for which a solar origin seemed violations unambiguously. A leading ple, the earliest x-ray data from small rocket inconsistent. Fortunately, the characteristics proposal for the detection of exo-at- probes and from satellites were often found of this event did not at all resemble those of a mospheric nuclear explosions was the use of to disagree significantly. The quality of the nuclear detonation, and thus the event did satellites with instruments that included de- data, rather than actual variations in the not create concern of a possible test-ban tectors sensitive to the gamma rays emitted sources, was suspected as the reason for treaty violation. by the explosion as well as those emitted these discrepancies. -
Advanced Approaches to High Intensity Laser-Driven Ion Acceleration
Advanced Approaches to High Intensity Laser-Driven Ion Acceleration Andreas Henig M¨unchen2010 Advanced Approaches to High Intensity Laser-Driven Ion Acceleration Andreas Henig Dissertation an der Fakult¨atf¨urPhysik der Ludwig{Maximilians{Universit¨at M¨unchen vorgelegt von Andreas Henig aus W¨urzburg M¨unchen, den 18. M¨arz2010 Erstgutachter: Prof. Dr. Dietrich Habs Zweitgutachter: Prof. Dr. Toshiki Tajima Tag der m¨undlichen Pr¨ufung:26. April 2010 Contents Contentsv List of Figures ix Abstract xiii Zusammenfassung xv 1 Introduction1 1.1 History and Previous Achievements...................1 1.2 Envisioned Applications.........................3 1.3 Thesis Outline...............................5 2 Theoretical Background9 2.1 Ionization.................................9 2.2 Relativistic Single Electron Dynamics.................. 14 2.2.1 Electron Trajectory in a Linearly Polarized Plane Wave.... 15 2.2.2 Electron Trajectory in a Circularly Polarized Plane Wave... 17 2.2.3 Electron Ejection from a Focussed Laser Beam......... 18 2.3 Laser Propagation in a Plasma..................... 18 2.4 Laser Absorption in Overdense Plasmas................. 20 2.4.1 Collisional Absorption...................... 20 2.4.2 Collisionless Absorption..................... 21 2.5 Ion Acceleration.............................. 22 2.5.1 Target Normal Sheath Acceleration (TNSA).......... 22 2.5.2 Shock Acceleration........................ 26 2.5.3 Radiation Pressure Acceleration / Light Sail / Laser Piston. 27 3 Experimental Methods I - High Intensity Laser Systems 33 3.1 Fundamentals of Ultrashort High Intensity Pulse Generation..... 33 vi CONTENTS 3.1.1 The Concept of Mode-Locking.................. 33 3.1.2 Time-Bandwidth Product.................... 37 3.1.3 Chirped Pulse Amplification................... 39 3.1.4 Optical Parametric Amplification (OPA)............ 40 3.2 Laser Systems Utilized for Ion Acceleration Studies......... -
Electron Radiated Power in Cyclotron Radiation Emission Spectroscopy Experiments
Electron Radiated Power in Cyclotron Radiation Emission Spectroscopy Experiments A. Ashtari Esfahani,1, ∗ V. Bansal,2 S. B¨oser,3 N. Buzinsky,4 R. Cervantes,1 C. Claessens,3 L. de Viveiros,5 P. J. Doe,1 M. Fertl,1 J. A. Formaggio,4 L. Gladstone,6 M. Guigue,2, y K. M. Heeger,7 J. Johnston,4 A. M. Jones,2 K. Kazkaz,8 B. H. LaRoque,2 M. Leber,9 A. Lindman,3 E. Machado,1 B. Monreal,6 E. C. Morrison,2 J. A. Nikkel,7 E. Novitski,1 N. S. Oblath,2 W. Pettus,1 R. G. H. Robertson,1 G. Rybka,1, z L. Salda~na,7 V. Sibille,4 M. Schram,2 P. L. Slocum,7 Y-H. Sun,6 J. R. Tedeschi,2 T. Th¨ummler,10 B. A. VanDevender,2 M. Wachtendonk,1 M. Walter,10 T. E. Weiss,4 T. Wendler,5 and E. Zayas4 (Project 8 Collaboration) 1Center for Experimental Nuclear Physics and Astrophysics and Department of Physics, University of Washington, Seattle, WA 98195, USA 2Pacific Northwest National Laboratory, Richland, WA 99354, USA 3Institut f¨urPhysik, Johannes-Gutenberg Universit¨atMainz, 55128 Mainz, Germany 4Laboratory for Nuclear Science, Massachusetts Institute of Technology, Cambridge, MA 02139, USA 5Department of Physics, Pennsylvania State University, State College, PA 16801, USA 6Department of Physics, Case Western Reserve University, Cleveland, OH 44106, USA 7Wright Laboratory, Department of Physics, Yale University, New Haven, CT 06520, USA 8Lawrence Livermore National Laboratory, Livermore, CA 94550, USA 9Department of Physics, University of California Santa Barbara, CA 93106, USA 10Institut f¨urKernphysik, Karlsruher Institut f¨urTechnologie, 76021 Karlsruhe, Germany (Dated: January 10, 2019) The recently developed technique of Cyclotron Radiation Emission Spectroscopy (CRES) uses frequency information from the cyclotron motion of an electron in a magnetic bottle to infer its kinetic energy. -
Radiative Processes from Energetic Particles II: Gyromagnetic Radiation
Hale COLLAGE 2017 Lecture 21 Radiative processes from energetic particles II: Gyromagnetic radiation Bin Chen (New Jersey Institute of Technology) Previous lectures 1) Magnetic reconnection and energy release 2) Particle acceleration and heating 3) Chromospheric evaporation, loop e- magnetic heating and cooling reconnection Following lectures: How to diagnose the e- accelerated particles and the environment? • What? • Where? How? Shibata et al. 1995 • When? Outline • Radiation from energetic particles • Bremsstrahlung à Previous lecture • Gyromagnetic radiation (“magnetobremsstrahlung”) à This lecture • Other radiative processes à Briefly in the next lecture • Coherent radiation, inverse Compton, nuclear processes • Suggested reading: • Synchrotron radiation: Chapter 5 of “Essential Radio Astronomy” by Condon & Ransom 2016 • Gyroresonance radiation: Chapter 5 of Gary & Keller 2004 • Gyrosynchrotron radiation: Dulk & Marsh 1982 • Next two lectures: Diagnosing flare energetic particles using radio and hard X-ray imaging spectroscopy 8/3/10 8/3/10 Radio'Emission' Radio'Emission' .'Thermal' bremsstrahlung'(eAp)' .' Gyrosynchrotron'radia5on'(eAB)' ..'Thermal' 'Plasma'radia5on'( bremsstrahlungwAw'(eAp)' )' .' Gyrosynchrotron'radia5on'(eAB)' .'Plasma'radia5on'( wAw)' Radiation from an accelerated charge LarmorLarmor'formulae:'radia5on'from'an'accelerated'charge'''formulae:'radia5on'from'an'accelerated'charge'' 2 2 2 2 dP q 2 2 2q 2 dP q 2 2 2q 2 Larmor formula: = 3 a sin θ P = 3 a d =4 c 3 a sin θ P3c= 3 a dΩΩ 4ππc 3c Rela5vis5c'Larmor'formulae''