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Analytical modelling of the expansion of a solid obstacle interacting with a radiative shock

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High Power Laser Science and Engineering 2018年第2期6卷 123-132页

作者： Th.Michel E.Falize B.Albertazzi G.Rigon Y.Sakawa T.Sano H.Shimogawara R.Kumar T.Morita C.Michaut A.Casner R Barroso P.Mabey Y.Kuramitsu S.Laffite L.Van Box Som G.Gregori R.Kodama N.Ozaki P.Tzeferacos D.Lamb M.Koenig luli-cnrs ecole polytechniquecea:universite paris-saclayupmc univ paris 06:sorbonne universites-f-91128 palaiseau cedexFrance cea damdifF-91297 ArpajonFrance cea saclay dsm/irfu/service d'astrophysiqueF-91191 Gif-sur-YvetteFrance institute of laser engineering osaka universitySuitaOsaka 565-0871Japan faculty of engineering sciences kyushu university6-1 Kasuga-KoenKasugaFukuoka 816-8580Japan luth observatoire de parispsl research universitycnrsuniversite paris diderotSorbonne Paris Cite92190 MeudonFrance universite de bordeaux-cnrs-cea celia UMR 5107F-33405 TalenceFrance gepi observatoire de parispsl research universitycnrsuniversite paris diderotSorbonne Paris Cite75014 ParisFrance graduate school of engineering osaka universitySuitaOsaka 565-0871Japan lerma observatoire de parispsl research universitycnrssorbonne universitesUPMC Univ.Paris 06F-75005 ParisFrance clarendon laboratory university of oxfordParks RoadOxford OX1 3PUUK flash center for computational science university of chicagoIL 60637USA

In this paper, we present a model characterizing the interaction of a radiative shock(RS) with a solid material, as described in a recent paper(Koenig et al., Phys. Plasmas, 24, 082707(2017)), the new model is then related to recent experiments performed on the GEKKO XII laser facility. The RS generated in a xenon gas cell propagates towards a solid obstacle that is ablated by radiation coming from the shock front and the radiative precursor, mimicking processes occurring in astrophysical phenomena. The model presented here calculates the dynamics of the obstacle expansion,which depends on several parameters, notably the geometry and the temperature of the shock. All parameters required for the model have been obtained from experiments. Good agreement between experimental data and the model is found when spherical geometry is taken into account. As a consequence, this model is a useful and easy tool to infer parameters from experimental data(such as the shock temperature), and also to design future experiments.

关键词： high energy density physics laser–plasmas interaction modelling plasmas astrophysics plasma physics radiative hydrodynamics radiative shock

Laboratory radiative accretion shocks on GEKKO XⅡlaser facility for POLAR project

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High Power Laser Science and Engineering 2018年第2期6卷 181-188页

作者： L.Van Box Som E.Falize M.Koenig Y.Sakawa B.Albertazzi E Barroso J.-***-Bidaud C.Busschaert A.Ciardi Y.Hara N.Katsuki R.Kumar E Lefevre C.Michaut Th.Michel T.Miura T.Morita M.Mouchet G.Rigon T.Sano S.Shiiba H.Shimogawara S.Tomiya CEA-DAM-DIF F-91297 ArpajonFrance LERMA Sorbonne UniversiteObservatoire de ParisUniversite PSLCNRSF-75005 ParisFrance CEA Saclay DSM/Irfu/Service d'AstrophysiqueF-91191 Gif-sur-YvetteFrance LULI-CNRS Ecole PolytechniqueCEA:Universite Paris-Saclay UPMC Univ Paris 06:Sorbonne Universite-F-91128 Palaiseau Cedex France Graduate School of Engineering Osaka UniversitySuitaOsaka 565-0871Japan Institute of Laser Engineering Osaka UniversitySuitaOsaka 565-0871Japan Faculty of Engineering Sciences Kyushu University6-1 Kasuga-KoenKasugaFukuoka 816-8580Japan Aoyama Gakuin University Japan GEPI Observatoire de ParisPSL Research UniversityCNRSUniversite Paris DiderotSorbonne Paris CiteF-75014 ParisFrance luth Observatoire de ParisPSL Research UniversityCNRSUniversite Paris DiderotSorbonne Paris CiteF-92195 MeudonFrance

A new target design is presented to model high-energy radiative accretion shocks in polars. In this paper, we present the experimental results obtained on the GEKKO XII laser facility for the POLAR project. The experimental results are compared with 2 D FCI2 simulations to characterize the dynamics and the structure of plasma flow before and after the collision. The good agreement between simulations and experimental data confirms the formation of a reverse shock where cooling losses start modifying the post-shock region. With the multi-material structure of the target,a hydrodynamic collimation is exhibited and a radiative structure coupled with the reverse shock is highlighted in both experimental data and simulations. The flexibility of the laser energy produced on GEKKO XII allowed us to produce high-velocity flows and study new and interesting radiation hydrodynamic regimes between those obtained on the LULI2000 and Orion laser facilities.

关键词： accretion processes high power laser hydrodynamics laboratory astrophysics

Experimental platform for the investigation of magnetized-reverse-shock dynamics in the context of POLAR

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High Power Laser Science and Engineering 2018年第3期6卷 36-49页

作者： B. Albertazzi E. Falize A. Pelka E Brack E Kroll R. Yurchak E. Brambrink E Mabey N. Ozaki S. Pikuz L. Van Box Som J. M. Bonnet-Bidaud J. E. Cross E. Filippov G. Gregori R. Kodama M. Mouchet T. Morita Y. Sakawa R. E Drake C. C. Kuranz M. J.-E. Manuel C. Li E Tzeferacos D. Lamb U. Schramm M. Koenig LULI- CNRS Ecole Polytechnique CEA: Universite Paris-Saclay UPMC Univ Paris 06: Sorbonne Universites- F-91128 Palaiseau cedex France CEA-DAM-DIF F-91297 Arpajon France CEA Saclay DSM/Irfu/Service d'Astrophysique F-91191 Gif-sur- Yvette France Helmholtz-Zentrum Dresden - Rossendorf HZDR Bautzner Landstrαβe 400 01328 Dresden Germany Department of Atmospheric Oceanic and Space Sciences University of Michigan Ann Arbor M148109 USA Graduate School of Engineering Osaka University Suita Osaka 565-0871 Japan JIHT-RAS 13-2 lzhorskaya st. Moscow 125412 Russia National Research Nuclear University MEPhl Moscow 115409 Russia Department of Physics University of Oxford Parks Road Oxford OX1 3PU UK Institute of Laser Engineering Osaka University Suita Osaka 565-0871 Japan luth Observatoire de Paris UMR CNRS 8102 Universite Paris Diderot 92190 Meudon France Department of Energy Engineering Science Faculty of Engineering Sciences Kyushu University Japan General Atomics San Diego CA 92121 USA Plasma Science and Fusion Center Massachusetts Institute of Technology 77 Massachusetts Avenue Cambridge MA 02139 USA Flash Center for Computational Science University of Chicago IL 60637 USA

The influence of a strong external magnetic field on the collimation of a high Mach number plasma flow and its collision with a solid obstacle is investigated experimentally and numerically. The laser irradiation(I ～ 2 × 10^(14) W · cm^(-2)) of a multilayer target generates a shock wave that produces a rear side plasma expanding flow. Immersed in a homogeneous10 T external magnetic field, this plasma flow propagates in vacuum and impacts an obstacle located a few mm from the main target. A reverse shock is then formed with typical velocities of the order of 15–20 ± 5 km/s. The experimental results are compared with 2 D radiative magnetohydrodynamic simulations using the FLASH code. This platform allows investigating the dynamics of reverse shock, mimicking the processes occurring in a cataclysmic variable of polar type.

关键词：磁场等离子体流变量激光技术

The Giant Radio Array for Neutrino Detection(GRAND):Science and design

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Science China(Physics,Mechanics & Astronomy) 2020年第1期63卷 5-47页

作者： Jaime álvarez-Mu?iz Rafael Alves Batista Aswathi Balagopal V. Julien Bolmont Mauricio Bustamante Washington Carvalho Jr. Didier Charrier Isma?l Cognard Valentin Decoene Peter B.Denton Sijbrand De Jong Krijn D.De Vries Ralph Engel Ke Fang Chad Finley Stefano Gabici Quan Bu Gou Jun Hua Gu Claire Guépin Hong Bo Hu Yan Huang Kumiko Kotera Sandra Le Coz Jean-Philippe Lenain Guo Liang Léü Olivier Martineau-Huynh Miguel Mostafá Fabrice Mottez Kohta Murase Valentin Niess Foteini Oikonomou Tanguy Pierog Xiang Li Qian Bo Qin Duan Ran Nicolas Renault-Tinacci Markus Roth Frank G.Schr ?der Fabian Schüssler Cyril Tasse Charles Timmerman Matías Tueros Xiang Ping Wu Philippe Zarka Andreas Zech B.Theodore Zhang Jian Li Zhang Yi Zhang Qian Zheng Anne Zilles SUBATECH Institut Mines-Telecom Atlantique – CNRS/IN2P3 – Université de Nantes Laboratoire de Physique et Chimie de l’Environnement et de l’Espace LPC2E CNRS-Université d’Orléans 12. Station de Radioastronomie de Nan?cay Observatoire de Paris Sorbonne Université UMR 7095 Institut d’Astrophysique de Paris Institute for Mathematics Astrophysics and Particle Physics (IMAPP) Radboud Universiteit Nationaal Instituut voor Kernfysica en Hoge Energie Fysica (NIKHEF) IIHE/ELEM Vrije Universiteit Brussel Institute for Nuclear Physics (IKP) Karlsruhe Institute of Technology (KIT) Einstein Fellow Stanford University Department of Astronomy University of Maryland Departamento de Física de Partículas & Instituto Galego de Física de Altas Enerxías Universidad de Santiago de Compostela Joint Space-Science Institute Oskar Klein Centre Stockholm University Department of Physics Stockholm University Astro Particule et Cosmologie (APC) Université Paris Diderot CNRS/IN2P3 CEA/Irfu Observatoire de Paris Institute of High Energy Physics Chinese Academy of Sciences National Astronomical Observatories Chinese Academy of Sciences School of Physical Science and Technology Xinjiang University Center for Particle and Gravitational Astrophysics Pennsylvania State University Department of Physics Pennsylvania State University Department of Astronomy & Astrophysics Pennsylvania State University Instituto de Astronomia Geofísica e Ciências Atmosféricas Universidade de S?o Paulo luth Observatoire de Paris CNRS Université Paris Diderot PSL Research University Clermont Université Université Blaise Pascal CNRS/IN2P3 Lab. de Physique Corpusculaire European Southern Observatory Department of Mechanical and Electrical Engineering Shandong Management University Bartol Research Institute Department of Physics and Astronomy University of Delaware IRFU CEA Université Paris-Saclay GEPI Observatoire de Paris CNRS Université Paris Diderot Instituto de F′?sica La P

The Giant Radio Array for Neutrino Detection(GRAND) is a planned large-scale observatory of ultra-high-energy(UHE) cosmic particles, with energies exceeding 10~8 Ge V. Its goal is to solve the long-standing mystery of the origin of UHE cosmic rays. To do this, GRAND will detect an unprecedented number of UHE cosmic rays and search for the undiscovered UHE neutrinos and gamma rays associated to them with unmatched sensitivity. GRAND will use large arrays of antennas to detect the radio emission coming from extensive air showers initiated by UHE particles in the atmosphere. Its design is modular: 20 separate, independent sub-arrays, each of 10000 radio antennas deployed over 10000 km~2. A staged construction plan will validate key detection techniques while achieving important science goals early. Here we present the science goals, detection strategy, preliminary design, performance goals, and construction plans for GRAND.

关键词： radio telescopes neutrinos in astronomical observations cosmic rays in astronomical observations radiowave radiation: sources galactic and extragalactic cosmic rays

The Giant Radio Array for Neutrino Detection(GRAND):Science and design

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Science China(Physics,Mechanics & Astronomy) 2020年第1期63卷 1-43页

作者： Jaime Alvarez-Muniz Rafael Alves Batista Aswathi Balagopal V. Julien Bolmont Mauricio Bustamante Washington Carvalho Jr. Didier Charrier Ismael Cognard Valentin Decoene Peter B.Denton Sijbrand De Jong Krijn D.De Vries Ralph Engel Ke Fang Chad Finley Stefano Gabici Quan Bu Gou Jun Hua Gu Claire Guépin Hong Bo Hu Yan Huang Kumiko Kotera Sandra Le Coz Jean-Philippe Lenain Guo Liang Léü Olivier Martineau-Huynh Miguel Mostafá Fabrice Mottez Kohta Murase Valentin Niess Foteini Oikonomou Tanguy Pierog Xiang Li Qian Bo Qin Duan Ran Nicolas Renault-Tinacci Markus Roth Frank G.Schroder Fabian Schüssler Cyril Tasse Charles Timmerman Matías Tueros Xiang Ping Wu Philippe Zarka Andreas Zech B.Theodore Zhang Jian Li Zhang Yi Zhang Qian Zheng Anne Zilles Departamento de Fisica de Particulas&lnstituto Galego de Fisica de Altas Enerxias Universidad de Santiago de CompostelaSantiago de Compostela 15782Spain Instituto de Astronomia Geofisica e Ciencias AtmosfericasUniversidade de Sao PauloSao Paulo-SP 05508-090Brazil Department of Physics-Astrophysics University of OxfordDWBOxford 0X13RHUK Institute of Experimental Particle Physics(ETP) Karlsruhe Institute of Technology(KIT)Karlsru he D-76021Germany Laboratoire de Physique Nucleeaire et de Hautes Energies(LPNHE) Sorbonne UniversiteUniversite Paris DiderotSorbonne Paris CiteCNRS place Jussieu F-75252Paris Cedex 5France Niels Bohr International Academy and DARK Niels Bohr InstituteCopenhagen 2100Denmark Discovery Center Niels Bohr InstituteCopenhagen 2100Denmark Center for Cosmology and AstroParticle Physics(CCA.PP)&Department of Physics Ohio State UniversityColumbus OH 43210USA Universidade de Santiago de Compostela Santiago de Compostela 15782Spain 0SUBATECH Institut Mines-Telecom Atlantique-CNRS/IN2P3-Universite de NantesNantes 44300France Laboratoire de Physique et Chimie de KEnvironnement et de VEspace LPC2E CNRS-Universite d'Orleans Orleans F-45071France Station de Radioastronomie de Nancay Observatoire de ParisCNRS/INSU F-18330 NangayFrance Sorbonne Universite UMR 7095Institut d'Astrophysique de Paris98 bis bd AragoParis 75014France Institute for Mathematics Astrophysics and Particle Physics(IMAPP)Radboud UniversiteitNijmegen 6500Netherlands Nationaal Instituut voor Kemfysica en Hoge Energie Fysica(NIKHEF) Amsterdam NL-1009Netherlands IIHE/ELEM Vrije Universiteit BrusselPleinlaan 2Brussels 1050Belgium Institute for Nuclear Physics(IKP) Karlsruhe Institute of Technology(KIT)Karlsruhe D-76021Germany Einstein Fellow Stanford UniversityStanford CA 94305USA Department of Astronomy University of MarylandCollege Park MD 20742-2421USA Joint Space-Science Institute College Park MD 20742-2421USA Oskar Klein Centre Stockholm UniversityStockholm SE-10691Sweden Department of Phy

The Giant Radio Array for Neutrino Detection(GRAND)is a planned large-scale observatory of ultra-high-energy(UHE)cosmic particles,with energies exceeding 10~8 Ge V.Its goal is to solve the long-standing mystery of the origin of UHE cosmic rays.To do this,GRAND will detect an unprecedented number of UHE cosmic rays and search for the undiscovered UHE neutrinos and gamma rays associated to them with unmatched sensitivity.GRAND will use large arrays of antennas to detect the radio emission coming from extensive air showers initiated by UHE particles in the atmosphere.Its design is modular:20 separate,independent sub-arrays,each of 10000 radio antennas deployed over 10000 km^2.A staged construction plan will validate key detection techniques while achieving important science goals early.Here we present the science goals,detection strategy,preliminary design,performance goals,and construction plans for GRAND.

关键词： radio telescopes neutrinos in astronomical observations cosmic rays in astronomical observations radiowave radiation:sources galactic and extragalactic cosmic rays:galactic and extragalactic