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51. Fast electron generation using PW-class PEARL facility

Author

Soloviev, A. A., Burdonov, K. F., Ginzburg, V. N., Gonoskov, A. A., Katin, E. V., Kim, A. V., Kirsanov, A. V., Korzhimanov, A. V., Kostyukov, I. Yu., Lozhkarev, V. V., Luchinin, G. A., Malshakov, A. N., Martyanov, M. V., Nerush, E. N., Palashov, O. V., Poteomkin, A. K., Sergeev, A. M., Shaykin, A. A., Starodubtsev, M. V., Yakovlev, I. V., Zelenogorsky, V. V., Khazanov, E. A., Soloviev, A. A., Burdonov, K. F., Ginzburg, V. N., Gonoskov, A. A., Katin, E. V., Kim, A. V., Kirsanov, A. V., Korzhimanov, A. V., Kostyukov, I. Yu., Lozhkarev, V. V., Luchinin, G. A., Malshakov, A. N., Martyanov, M. V., Nerush, E. N., Palashov, O. V., Poteomkin, A. K., Sergeev, A. M., Shaykin, A. A., Starodubtsev, M. V., Yakovlev, I. V., Zelenogorsky, V. V., and Khazanov, E. A.

Abstract

We use a PW-class PEARL facility to study fast electron beam generation during high intensity laser pulse interaction with a supersonic gas jet. We show that electron beams with several hundreds of MeV and relatively large charges, of hundreds of pC and more, can be effectively produced without any guiding structures. PIC simulations also confirm the obtained experimental data and provide optimized conditions of laser–plasma interaction for high-charged beam production.

Published
2011
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54. Detailed characterization of laboratory magnetized super-critical collisionless shock and of the associated proton energization

Author

W. Yao, A. Fazzini, S. N. Chen, K. Burdonov, P. Antici, J. Béard, S. Bolaños, A. Ciardi, R. Diab, E. D. Filippov, S. Kisyov, V. Lelasseux, M. Miceli, Q. Moreno, V. Nastasa, S. Orlando, S. Pikuz, D. C. Popescu, G. Revet, X. Ribeyre, E. d’Humières, J. Fuchs, Laboratoire pour l'utilisation des lasers intenses (LULI), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-École polytechnique (X)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Horia Hulubei National Institute for Physics and Nuclear Engineering, IAP, Russian Academy of Sciences, 603155, Nizhny Novgorod, Russia, Énergie Matériaux Télécommunications - INRS (EMT-INRS), Institut National de la Recherche Scientifique [Québec] (INRS)-Université du Québec à Montréal = University of Québec in Montréal (UQAM), Laboratoire national des champs magnétiques intenses - Toulouse (LNCMI-T), Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Université de Toulouse (UT)-Institut National des Sciences Appliquées (INSA)-Université de Toulouse (UT)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Joint Institute for High Temperatures of the RAS (JIHT), Russian Academy of Sciences [Moscow] (RAS), Università degli studi di Palermo - University of Palermo, INAF - Osservatorio Astronomico di Palermo (OAPa), Istituto Nazionale di Astrofisica (INAF), Centre d'Etudes Lasers Intenses et Applications (CELIA), Université de Bordeaux (UB)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS), Institute of Physics of the Czech Academy of Sciences (FZU / CAS), Czech Academy of Sciences [Prague] (CAS), Moscow State Engineering Physics Institute (MEPhI), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université de Bordeaux (UB), Yao W., Fazzini A., Chen S.N., Burdonov K., Antici P., Beard J., Bolanos S., Ciardi A., Diab R., Filippov E.D., Kisyov S., Lelasseux V., Miceli M., Moreno Q., Nastasa V., Orlando S., Pikuz S., Popescu D.C., Revet G., Ribeyre X., D'Humieres E., and Fuchs J.

Subjects
Nuclear and High Energy Physics, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, magnetic field, QC770-798, shock waves, 01 natural sciences, Atomic and Molecular Physics, and Optics, Physics - Plasma Physics, 010305 fluids & plasmas, Plasma Physics (physics.plasm-ph), Settore FIS/05 - Astronomia E Astrofisica, Nuclear Energy and Engineering, [PHYS.PHYS.PHYS-PLASM-PH]Physics [physics]/Physics [physics]/Plasma Physics [physics.plasm-ph], Nuclear and particle physics. Atomic energy. Radioactivity, 0103 physical sciences, Physics::Space Physics, Electrical and Electronic Engineering, 010306 general physics
Abstract

Collisionless shocks are ubiquitous in the Universe and are held responsible for the production of nonthermal particles and high-energy radiation. In the absence of particle collisions in the system, theory shows that the interaction of an expanding plasma with a pre-existing electromagnetic structure (as in our case) is able to induce energy dissipation and allow shock formation. Shock formation can alternatively take place when two plasmas interact, through microscopic instabilities inducing electromagnetic fields that are able in turn to mediate energy dissipation and shock formation. Using our platform in which we couple a rapidly expanding plasma induced by high-power lasers (JLF/Titan at LLNL and LULI2000) with high-strength magnetic fields, we have investigated the generation of a magnetized collisionless shock and the associated particle energization. We have characterized the shock as being collisionless and supercritical. We report here on measurements of the plasma density and temperature, the electromagnetic field structures, and the particle energization in the experiments, under various conditions of ambient plasma and magnetic field. We have also modeled the formation of the shocks using macroscopic hydrodynamic simulations and the associated particle acceleration using kinetic particle-in-cell simulations. As a companion paper to Yao et al. [Nat. Phys. 17, 1177–1182 (2021)], here we show additional results of the experiments and simulations, providing more information to allow their reproduction and to demonstrate the robustness of our interpretation of the proton energization mechanism as being shock surfing acceleration.

Published
2022
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55. Inferring possible magnetic field strength of accreting inflows in EXor-type objects from scaled laboratory experiments

Author

Mikhail Gushchin, Rosaria Bonito, K. Gubskiy, Efim A. Khazanov, Julien Fuchs, A. V. Strikovskiy, V. I. Gundorin, A. Kuznetsov, S. N. Ryazantsev, S. A. Pikuz, Salvatore Orlando, Alexander Soloviev, W. P. Yao, I. Shaykin, Teresa Giannini, R. Zemskov, Ivan V. Yakovlev, Shihua Chen, N. A. Aidakina, I. Zudin, Andrey Shaykin, M. V. Starodubtsev, Vladislav Ginzburg, K. Burdonov, A. A. Kuzmin, J. Béard, G. Revet, A. A. Kochetkov, Andrea Ciardi, S. V. Korobkov, Costanza Argiroffi, Laboratoire pour l'utilisation des lasers intenses (LULI), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-École polytechnique (X)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Laboratoire national des champs magnétiques intenses - Toulouse (LNCMI-T), Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Université de Toulouse (UT)-Institut National des Sciences Appliquées (INSA)-Université de Toulouse (UT)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Institute of Applied Physics of RAS, Russian Academy of Sciences [Moscow] (RAS), INAF - Osservatorio Astronomico di Palermo (OAPa), Istituto Nazionale di Astrofisica (INAF), INAF - Osservatorio Astronomico di Roma (OAR), Università degli studi di Palermo - University of Palermo, Horia Hulubei National Institute for Physics and Nuclear Engineering, Moscow State Engineering Physics Institute (MEPhI), Joint Institute for High Temperatures of the RAS (JIHT), The National Research Nuclear University MEPhI (Moscow Engineering Physics Institute) [Moscow, Russia], This work was partly done within the LABEX Plas@Par, the DIM ACAV funded by the Region Ile-de-France, and supported by Grant No. 11-IDEX- 0004-02 from ANR, The research leading to these results is supported by Extreme Light Infrastructure Nuclear Physics (ELINP) Phase II, a project co-financed by the Romanian Government and European Union through the European Regional Development Fund, and by the project ELI-RO-2020-23 funded by IFA (Romania)., European Project: ERC787539,GENESIS, Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), HEP, INSPIRE, Burdonov K., Bonito R., Giannini T., Aidakina N., Argiroffi C., Beard J., Chen S.N., Ciardi A., Ginzburg V., Gubskiy K., Gundorin V., Gushchin M., Kochetkov A., Korobkov S., Kuzmin A., Kuznetsov A., Pikuz S., Revet G., Ryazantsev S., Shaykin A., Shaykin I., Soloviev A., Starodubtsev M., Strikovskiy A., Yao W., Yakovlev I., Zemskov R., Zudin I., Khazanov E., Orlando S., and Fuchs J.

Subjects
Shock wave, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Field strength, Astrophysics, stars: pre-main sequence, 01 natural sciences, magnetohydrodynamics (MHD), Settore FIS/05 - Astronomia E Astrofisica, accretion, 0103 physical sciences, Protostar, Astrophysics::Solar and Stellar Astrophysics, 010306 general physics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, [PHYS]Physics [physics], accretion disks, Astronomy and Astrophysics, Radius, Plasma, shock waves, Accretion, accretion disks, Accretion (astrophysics), Magnetic field, T Tauri star, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, instabilities, stars: individual: V1118 Ori, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

Aims. EXor-type objects are protostars that display powerful UV-optical outbursts caused by intermittent and powerful events of magnetospheric accretion. These objects are not yet well investigated and are quite difficult to characterize. Several parameters, such as plasma stream velocities, characteristic densities, and temperatures, can be retrieved from present observations. As of yet, however, there is no information about the magnetic field values and the exact underlying accretion scenario is also under discussion. Methods. We use laboratory plasmas, created by a high power laser impacting a solid target or by a plasma gun injector, and make these plasmas propagate perpendicularly to a strong external magnetic field. The propagating plasmas are found to be well scaled to the presently inferred parameters of EXor-type accretion event, thus allowing us to study the behaviour of such episodic accretion processes in scaled conditions. Results. We propose a scenario of additional matter accretion in the equatorial plane, which claims to explain the increased accretion rates of the EXor objects, supported by the experimental demonstration of effective plasma propagation across the magnetic field. In particular, our laboratory investigation allows us to determine that the field strength in the accretion stream of EXor objects, in a position intermediate between the truncation radius and the stellar surface, should be of the order of 100 G. This, in turn, suggests a field strength of a few kilogausses on the stellar surface, which is similar to values inferred from observations of classical T Tauri stars.

Published
2021
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56. Laboratory evidence for proton energization by collisionless shock surfing

Author

G. Revet, K. Burdonov, J. Béard, A. Fazzini, E. D. Filippov, S. Bolaños, Julien Fuchs, V. Lelasseux, S. A. Pikuz, D. C. Popescu, Salvatore Orlando, W. P. Yao, V. Nastasa, Patrizio Antici, Andrea Ciardi, S. Kisyov, Quentin Moreno, Marco Miceli, Xavier Ribeyre, Emmanuel d'Humières, R. Diab, Sophia Chen, Laboratoire pour l'utilisation des lasers intenses (LULI), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-École polytechnique (X)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Laboratoire national des champs magnétiques intenses - Toulouse (LNCMI-T), Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Université de Toulouse (UT)-Institut National des Sciences Appliquées (INSA)-Université de Toulouse (UT)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Centre d'Etudes Lasers Intenses et Applications (CELIA), Université de Bordeaux (UB)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS), ITA, FRA, CAN, CZE, ROU, RUS, Yao W., Fazzini A., Chen S.N., Burdonov K., Antici P., Beard J., Bolanos S., Ciardi A., Diab R., Filippov E.D., Kisyov S., Lelasseux V., Miceli M., Moreno Q., Nastasa V., Orlando S., Pikuz S., Popescu D.C., Revet G., Ribeyre X., d'Humieres E., Fuchs J., Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), and Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université de Bordeaux (UB)

Subjects
Shock wave, Proton, Astrophysics::High Energy Astrophysical Phenomena, General Physics and Astronomy, FOS: Physical sciences, 01 natural sciences, Acceleration, Settore FIS/05 - Astronomia E Astrofisica, 0103 physical sciences, Bow shock (aerodynamics), 010306 general physics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Mechanics, plasmas, Physics - Plasma Physics, Charged particle, Computer Science::Computers and Society, [PHYS.PHYS.PHYS-GEN-PH]Physics [physics]/Physics [physics]/General Physics [physics.gen-ph], Magnetic field, Shock (mechanics), Plasma Physics (physics.plasm-ph), Supernova, 13. Climate action, Physics::Space Physics, Physics::Accelerator Physics
Abstract

Charged particles can be accelerated to high energies by collisionless shock waves in astrophysical environments, such as supernova remnants. By interacting with the magnetized ambient medium, these shocks can transfer energy to particles. Despite increasing efforts in the characterization of these shocks from satellite measurements at Earth’s bow shock as well as powerful numerical simulations, the underlying acceleration mechanism or a combination thereof is still widely debated. Here we show that astrophysically relevant super-critical quasi-perpendicular magnetized collisionless shocks can be produced and characterized in the laboratory. We observe the characteristics of super-criticality in the shock profile as well as the energization of protons picked up from the ambient gas to hundreds of kiloelectronvolts. Kinetic simulations modelling the laboratory experiment identified shock surfing as the proton acceleration mechanism. Our observations not only provide direct evidence of early-stage ion energization by collisionless shocks but also highlight the role played by this particular mechanism in energizing ambient ions to feed further stages of acceleration. Furthermore, our results open the door to future laboratory experiments investigating the possible transition to other mechanisms, when increasing the magnetic field strength, or the effect that induced shock front ripples could have on acceleration processes. Proton acceleration by a super-critical collisionless shock is observed in laboratory experiments, and numerical simulations suggest shock surfing as the underlying acceleration mechanism.

Published
2021
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57. Laboratory evidence for asymmetric accretion structure upon slanted matter impact in young stars

Author

Rosaria Bonito, Salvatore Orlando, O. Willi, Julien Fuchs, S. N. Chen, K. F. Burdonov, Mirela Cerchez, J. Béard, G. Revet, S. A. Pikuz, M. V. Starodubtsev, Rafael L. Rodríguez, E. D. Filippov, Costanza Argiroffi, Andrea Ciardi, G. Espinosa, S. Bolanos, Michal Smid, Laboratoire pour l'utilisation des lasers intenses (LULI), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-École polytechnique (X)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire national des champs magnétiques intenses - Toulouse (LNCMI-T), Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Burdonov K., Revet G., Bonito R., Argiroffi C., Beard J., Bolanos S., Cerchez M., Chen S.N., Ciardi A., Espinosa G., Filippov E., Pikuz S., Rodriguez R., Smid M., Starodubtsev M., Willi O., Orlando S., Fuchs J., Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), INAF - Osservatorio Astronomico di Palermo (OAPa), Istituto Nazionale di Astrofisica (INAF), Università degli studi di Palermo - University of Palermo, Heinrich Heine Universität Düsseldorf = Heinrich Heine University [Düsseldorf], Horia Hulubei National Institute for Physics and Nuclear Engineering, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Universidad de las Palmas de Gran Canaria (ULPGC), Joint Institute for High Temperatures of the RAS (JIHT), Russian Academy of Sciences [Moscow] (RAS), Institute of Applied Physics (IAP, Nizhny Novgorod), Moscow State Engineering Physics Institute (MEPhI), Helmholtz-Zentrum Dresden-Rossendorf (HZDR), This work was partly done within the LABEX Plas@Par, the DIM ACAV funded by the Region Ilede-France, This work was supported by Grant No. 11-IDEX- 0004-02 from ANR (France), ANR-12-BS09-0025,SILAMPA,Simuler en laboratoire des écoulements de plasmas magnétisés pour l'astrophysique(2012), European Project: ERC787539,GENESIS, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Institut National des Sciences Appliquées (INSA)-Université de Toulouse (UT)-Institut National des Sciences Appliquées (INSA)-Université de Toulouse (UT)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), and Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Shock wave, stars, Accretion, Magnetohydrodynamics (MHD), Young stellar object, FOS: Physical sciences, X-rays: stars, Astrophysics, 01 natural sciences, Shock waves, Settore FIS/05 - Astronomia E Astrofisica, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010306 general physics, Ejecta, 010303 astronomy & astrophysics, Chromosphere, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, pre-main sequence -X-rays, Astronomy and Astrophysics, Plasma, Planetary system, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], accretion disks -instabilities -magnetohydrodynamics (MHD) -shock waves -stars, Accretion (astrophysics), Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Instabilities, Accretion disks, Stars: pre-main sequence, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

Aims. Investigating the process of matter accretion onto forming stars through scaled experiments in the laboratory is important in order to better understand star and planetary system formation and evolution. Such experiments can indeed complement observations by providing access to the processes with spatial and temporal resolution. A previous investigation revealed the existence of a two-component stream: a hot shell surrounding a cooler inner stream. The shell was formed by matter laterally ejected upon impact and refocused by the local magnetic field. That laboratory investigation was limited to normal incidence impacts. However, in young stellar objects, the complex structure of magnetic fields causes variability of the incident angles of the accretion columns. This led us to undertake an investigation, using laboratory plasmas, of the consequence of having a slanted accretion impacting a young star. Methods. Here, we used high power laser interactions and strong magnetic field generation in the laboratory, complemented by numerical simulations, to study the asymmetry induced upon accretion structures when columns of matter impact the surface of young stars with an oblique angle. Results. Compared to the scenario where matter accretes perpendicularly to the star surface, we observe a strongly asymmetric plasma structure, strong lateral ejecta of matter, poor confinement of the accreted material, and reduced heating compared to the normal incidence case. Thus, slanted accretion is a configuration that seems to be capable of inducing perturbations of the chromosphere and hence possibly influencing the level of activity of the corona.

Published
2020
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58. Characterization and performance of the Apollon Short-Focal-Area facility following its commissioning at 1 PW level

Author

A. Chaleil, Jean-Luc Paillard, Y. Ayoul, A. Beluze, W. P. Yao, F. Negoita, A. Leblanc, Julien Fuchs, Xavier Davoine, V. Lelasseux, G. Qi, A. Fazzini, Fabrizio Consoli, N. Lebas, F. Perez, A. Freneaux, S. A. Pikuz, J. P. Delaneau, L. Lecherbourg, Emmanuel d'Humières, V. Horny, P.-A. Söderström, E. D. Filippov, Sophia Chen, D. Cavanna, Patrick Audebert, J. L. Dubois, M. Chabanis, F. Mathieu, Patrizio Antici, Zhi-wei Chen, Fabien Quéré, T. Ceccotti, L. Lancia, J. Albrecht, P. Forestier-Colleoni, W. Ma, M. Cuciuc, Laurent Gremillet, M. Scisciò, S. Vallières, Camille Evrard, Lucas Ranc, Shuhui Sun, Dimitris N. Papadopoulos, K. Burdonov, Luc Martin, P. Wang, Laboratoire pour l'utilisation des lasers intenses (LULI), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-École polytechnique (X)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Énergie Matériaux Télécommunications - INRS (EMT-INRS), Institut National de la Recherche Scientifique [Québec] (INRS)-Université du Québec à Montréal = University of Québec in Montréal (UQAM), Physique à Haute Intensité (PHI), Institut Rayonnement Matière de Saclay (IRAMIS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Laboratoire Interactions, Dynamiques et Lasers (ex SPAM) (LIDyl), Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), CEA- Saclay (CEA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Horia Hulubei National Institute of Physics and Nuclear Engineering (NIPNE), IFIN-HH, Agenzia Nazionale per le nuove Tecnologie, l’energia e lo sviluppo economico sostenibile (ENEA), Centre d'Etudes Lasers Intenses et Applications (CELIA), Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université de Bordeaux (UB), Joint Institute for High Temperatures of the RAS (JIHT), Russian Academy of Sciences [Moscow] (RAS), Laboratoire d'optique appliquée (LOA), École Nationale Supérieure de Techniques Avancées (ENSTA Paris)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), State Key Laboratory of Nuclear Physics and Technology (SKL-NPT), Peking University [Beijing], Burdonov, Konstantin, Laboratoire Interactions, Dynamiques et Lasers (ex SPAM) (LIDyl), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Laboratoire Matière sous Conditions Extrêmes (LMCE), DAM Île-de-France (DAM/DIF), Direction des Applications Militaires (DAM), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Direction des Applications Militaires (DAM), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Italian National agency for new technologies, Energy and sustainable economic development [Frascati] (ENEA), Université de Bordeaux (UB)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS), A.M.Obukhov Institute of Atmospheric Physics (IAP), Laboratoire Charles Fabry / Lasers, Laboratoire Charles Fabry (LCF), Institut d'Optique Graduate School (IOGS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Institut d'Optique Graduate School (IOGS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Thales LAS France, Institut National de la Recherche Scientifique [Québec] (INRS), ANR-17-CE30-0026,PiNNaCLE,Développement d'une ligne de neutrons pulsés compacte et de haute brillance(2017), European Project: 787539,GENESIS - 10.3030/787539, European Project: 633053,H2020,EURATOM-Adhoc-2014-20,EUROfusion(2014), Burdonov, K., Fazzini, A., Lelasseux, V., Albrecht, J., Antici, P., Ayoul, Y., Beluze, A., Cavanna, D., Ceccotti, T., Chabanis, M., Chaleil, A., Chen, S. N., Chen, Z., Consoli, F., Cuciuc, M., Davoine, X., Delaneau, J. P., D'Humieres, E., Dubois, J. -L., Evrard, C., Filippov, E., Freneaux, A., Forestier-Colleoni, P., Gremillet, L., Horny, V., Lancia, L., Lecherbourg, L., Lebas, N., Leblanc, A., Ma, W., Martin, L., Negoita, F., Paillard, J. -L., Papadopoulos, D., Perez, F., Pikuz, S., Qi, G., Quere, F., Ranc, L., Soderstrom, P. -A., Scisciò, M., Sun, S., Vallieres, S., Wang, P., Yao, W., Mathieu, F., Audebert, P., and Fuchs, J.

Subjects
Nuclear and High Energy Physics, Materials science, Phase (waves), FOS: Physical sciences, QC770-798, 01 natural sciences, Electromagnetic radiation, 010305 fluids & plasmas, law.invention, [PHYS] Physics [physics], Optics, law, Nuclear and particle physics. Atomic energy. Radioactivity, 0103 physical sciences, Irradiation, Electrical and Electronic Engineering, 010306 general physics, ComputingMilieux_MISCELLANEOUS, [PHYS]Physics [physics], business.industry, Laser, Atomic and Molecular Physics, and Optics, Physics - Plasma Physics, Characterization (materials science), Intensity (physics), Plasma Physics (physics.plasm-ph), Nuclear Energy and Engineering, business, Beam (structure), Nominal power (photovoltaic)
Abstract

We present the results of the first commissioning phase of the ``short focal length'' area (SFA) of the Apollon laser facility (located in Saclay, France), which was performed with the first available laser beam (F2), scaled to a nominal power of one petawatt. Under the conditions that were tested, this beam delivered on target pulses of 10 J average energy and 24 fs duration. Several diagnostics were fielded to assess the performance of the facility. The on-target focal spot, its spatial stability, the temporal intensity profile prior to the main pulse, as well as the resulting density gradient formed at the irradiated side of solid targets, have been thoroughly characterized, with the goal of helping users design future experiments. Emissions of energetic electrons, ions, and electromagnetic radiation were recorded, showing good laser-to-target coupling efficiency and an overall performance comparable with that of similar international facilities. This will be followed in 2022 by a further commissioning stage at the multi-petawatt level.

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59. Laboratory unraveling of matter accretion in young stars.

Author

Revet G, Chen SN, Bonito R, Khiar B, Filippov E, Argiroffi C, Higginson DP, Orlando S, Béard J, Blecher M, Borghesi M, Burdonov K, Khaghani D, Naughton K, Pépin H, Portugall O, Riquier R, Rodriguez R, Ryazantsev SN, Yu Skobelev I, Soloviev A, Willi O, Pikuz S, Ciardi A, and Fuchs J

Abstract

Accretion dynamics in the formation of young stars is still a matter of debate because of limitations in observations and modeling. Through scaled laboratory experiments of collimated plasma accretion onto a solid in the presence of a magnetic field, we open a first window on this phenomenon by tracking, with spatial and temporal resolution, the dynamics of the system and simultaneously measuring multiband emissions. We observe in these experiments that matter, upon impact, is ejected laterally from the solid surface and then refocused by the magnetic field toward the incoming stream. This ejected matter forms a plasma shell that envelops the shocked core, reducing escaped x-ray emission. This finding demonstrates one possible structure reconciling current discrepancies between mass accretion rates derived from x-ray and optical observations, respectively.

Published
2017
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