Collisionless Shocks Driven by Supersonic Plasma Flows with Self-Generated Magnetic Fieldsdoi:10.7910/DVN/KM45SYHarvard Dataverse2019-11-211C. K. Li, V. T. Tikhonchuk, , Q. Moreno, H. Sio, E. D’Humieres, X. Ribeyre, Ph. Korneev, S. Atzeni, R. Betti, A. Birkel, E. M. Campbell, R. K. Follett, J. A. Frenje, S. X. Hu, M. Koenig, Y. Sakawa, T. C. Sangster, F. H. Seguin, H. Takabe, S. Zhang, , R. D. Petrasso, 2019, "Collisionless Shocks Driven by Supersonic Plasma Flows with Self-Generated Magnetic Fields", https://doi.org/10.7910/DVN/KM45SY, Harvard Dataverse, V1Collisionless Shocks Driven by Supersonic Plasma Flows with Self-Generated Magnetic Fieldsdoi:10.7910/DVN/KM45SYC. K. Li, V. T. Tikhonchuk, , Q. Moreno, H. Sio, E. D’Humieres, X. Ribeyre, Ph. Korneev, S. Atzeni, R. Betti, A. Birkel, E. M. Campbell, R. K. Follett, J. A. Frenje, S. X. Hu, M. Koenig, Y. Sakawa, T. C. Sangster, F. H. Seguin, H. Takabe, S. Zhang, , R. D. PetrassoHarvard DataversePhysicsCollisionless shocksgasbaglaboratory astrophysicsmagnetized shocksplasma jetself-generated magnetic fieldsweibel instabilityCollisionless shocks are ubiquitous in the Universe as a consequence of supersonic plasma flows sweeping through interstellar and intergalactic media. These shocks are the cause of many observed astrophysical phenomena, but details of shock structure and behavior remain controversial because of the lack of ways to study them experimentally. Laboratory experiments reported here, with astrophysically relevant plasma parameters, demonstrate for the first time the formation of a quasiperpendicular magnetized collisionless shock. In the upstream it is fringed by a filamented turbulent region, a rudiment for a secondary Weibel-driven shock. This turbulent structure is found responsible for electron acceleration to energies exceeding the average energy by two orders of magnitude.<a href="http://library.psfc.mit.edu/catalog/reports/2010/19ja/19ja021/abstract.php">PSFC REPORT PSFC/JA-19-21</a><br /><br />The experiments were supported in part by grants from U.S. DOE (No. DE-0002949), Laboratory for Laser Energetics (No. 416107-G), National Laser User Facility (No. DE-NA000 3539), LLNL (No. B63159), and French National Research Agency (No. ANR-14-CE33-0019 MACH). Numerical simulations were supported in part by U.S. DOE NNSA ASC Grant No. 57789 to Argonne National Laboratory and by the HPC resources of CINES under allocation 2017-056129 made by Grand Equipment National de Calcul Intensif. Additional support was provided by European Research Council under the Seventh Framework Program (FP7/2007-2013) and Grants No. 256973 and No. 247039; ELI Tools for Advanced Simulation CZ.02.1.01/0.0/0.0/16_013/0001793 from the European Regional Development Fund; the MEPhI Academic Excellence Project (No. 02.a03.21.0005, 27.08.2013); and JSPS KAKENHI Grant No. 17H06202.This dataset is made available without information on how it can be used. You should communicate with the Contact(s) specified before use.19ja021_archival_manuscript.pdfapplication/pdf