TY - GEN A1 - Bohdan, Artem A1 - Niemiec, Jacek A1 - Kobzar, Oleh A1 - Pohl, Martin T1 - Erratum: Electron Pre-acceleration at Nonrelativistic High-Mach-number Perpendicular Shocks (The astrophysical journal : an international review of spectroscopy and astronomical physics. - Vol 847, 2017, 71) T2 - The astrophysical journal : an international review of spectroscopy and astronomical physics Y1 - 2019 U6 - https://doi.org/10.3847/1538-4357/ab2f89 SN - 0004-637X SN - 1538-4357 VL - 880 IS - 1 PB - IOP Publ. Ltd. CY - Bristol ER - TY - JOUR A1 - Jao, Chun-Sung A1 - Vafin, Sergei A1 - Chen, Ye A1 - Gross, Matthias A1 - Krasilnikov, Mikhail A1 - Loisch, Gregor A1 - Mehrling, Timon A1 - Niemiec, Jacek A1 - Oppelt, Anne A1 - de la Ossa, Alberto Martinez A1 - Osterhoff, Jens A1 - Pohl, Martin A1 - Stephan, Frank T1 - Preliminary study for the laboratory experiment of cosmic-rays driven magnetic field amplification JF - High Energy Density Physics N2 - To understand astrophysical magnetic-field amplification, we conducted a feasibility study for a laboratory experiment of a non-resonant streaming instability at the Photo Injector Test Facility at DESY, Zeuthen site (PITZ). This non-resonant streaming instability, also known as Bell’s instability, is generally regarded as a candidate for the amplification of interstellar magnetic field in the upstream region of supernova-remnant shocks, which is crucial for the efficiency of diffusive shock acceleration. In the beam-plasma system composed of a radio-frequency electron gun and a gas-discharge plasma cell, the goal of our experiment is to demonstrate the development of the non-resonant streaming instability and to find its saturation level in the laboratory environment. Since we find that the electron beam will be significantly decelerated on account of an electrostatic streaming instability, which will decrease the growth rate of desired non-resonant streaming instability, we discuss possible ways to suppress the electrostatic streaming instability by considering the characteristics of a field-emission-based quasi continuous-wave electron beam. KW - Laboratory astrophysics KW - Beam-plasma instability KW - Magnetic field amplification KW - Radio-frequency electron gun KW - Field-emission-based quasi continuous-wave electron beam Y1 - 2019 U6 - https://doi.org/10.1016/j.hedp.2019.04.001 SN - 1574-1818 SN - 1878-0563 VL - 32 SP - 31 EP - 43 PB - Elsevier CY - Amsterdam ER - TY - JOUR A1 - Iwamoto, Masanori A1 - Amano, Takanobu A1 - Hoshino, Masahiro A1 - Matsumoto, Yosuke A1 - Niemiec, Jacek A1 - Ligorini, Arianna A1 - Kobzar, Oleh A1 - Pohl, Martin T1 - Precursor Wave Amplification by Ion-Electron Coupling through Wakefield in Relativistic Shocks JF - The astrophysical journal : an international review of spectroscopy and astronomical physics ; Part 2, Letters N2 - We investigated electromagnetic precursor wave emission in relativistic shocks by using two-dimensional particle-in-cell simulations. We found that the wave amplitude is significantly enhanced by a positive feedback process associated with ion-electron coupling through the wakefields for high magnetization. The wakefields collapse during the nonlinear process of the parametric decay instability in the near-upstream region, where nonthermal electrons and ions are generated. The intense coherent emission and the particle acceleration may operate in high-energy astrophysical objects. Y1 - 2019 U6 - https://doi.org/10.3847/2041-8213/ab4265 SN - 2041-8205 SN - 2041-8213 VL - 883 IS - 2 PB - IOP Publ. Ltd. CY - Bristol ER - TY - JOUR A1 - Bohdan, Artem A1 - Niemiec, Jacek A1 - Pohl, Martin A1 - Matsumoto, Yosuke A1 - Amano, Takanobu A1 - Hoshino, Masahiro T1 - Kinetic Simulations of Nonrelativistic Perpendicular Shocks of Young Supernova Remnants. II. Influence of Shock-surfing Acceleration on Downstream Electron Spectra JF - The astrophysical journal : an international review of spectroscopy and astronomical physics N2 - We explore electron preacceleration at high-Mach-number nonrelativistic perpendicular shocks at, e.g., young supernova remnants, which are a prerequisite of further acceleration to very high energies via diffusive shock acceleration. Using fully kinetic particle-in-cell simulations of shocks and electron dynamics in them, we investigate the influence of shock-surfing acceleration (SSA) at the shock foot on the nonthermal population of electrons downstream of the shock. The SSA is followed by further energization at the shock ramp where the Weibel instability spawns a type of second-order Fermi acceleration. The combination of these two processes leads to the formation of a nonthermal electron population, but the importance of SSA becomes smaller for larger ion-to-electron mass ratios in the simulation. We discuss the resulting electron spectra and the relevance of our results to the physics of systems with real ion-to-electron mass ratios and fully three-dimensional behavior. KW - Shocks KW - Space plasmas KW - Supernova remnants KW - Interstellar medium Y1 - 2019 U6 - https://doi.org/10.3847/1538-4357/ab43cf SN - 0004-637X SN - 1538-4357 VL - 885 IS - 1 PB - IOP Publ. Ltd. CY - Bristol ER - TY - JOUR A1 - Nishikawa, Ken-Ichi A1 - Mizuno, Yosuke A1 - Gomez, Jose L. A1 - Duţan, Ioana A1 - Meli, Athina A1 - Niemiec, Jacek A1 - Kobzar, Oleh A1 - Pohl, Martin A1 - Sol, Hélène A1 - MacDonald, Nicholas A1 - Hartmann, Dieter H. T1 - Relativistic jet simulations of the weibel instability in the slab model to cylindrical jets with helical magnetic fields JF - Galaxies : open access journal N2 - The particle-in-cell (PIC) method was developed to investigate microscopic phenomena, and with the advances in computing power, newly developed codes have been used for several fields, such as astrophysical, magnetospheric, and solar plasmas. PIC applications have grown extensively, with large computing powers available on supercomputers such as Pleiades and Blue Waters in the US. For astrophysical plasma research, PIC methods have been utilized for several topics, such as reconnection, pulsar dynamics, non-relativistic shocks, relativistic shocks, and relativistic jets. PIC simulations of relativistic jets have been reviewed with emphasis placed on the physics involved in the simulations. This review summarizes PIC simulations, starting with the Weibel instability in slab models of jets, and then focuses on global jet evolution in helical magnetic field geometry. In particular, we address kinetic Kelvin-Helmholtz instabilities and mushroom instabilities. KW - particle-in-cell simulations KW - relativistic jets KW - the Weibel instability KW - kink-like instability KW - mushroom instability KW - global jets KW - helical magnetic fields KW - recollimation shocks Y1 - 2019 U6 - https://doi.org/10.3390/galaxies7010029 SN - 2075-4434 VL - 7 IS - 1 PB - MDPI CY - Basel ER - TY - JOUR A1 - Bohdan, Artem A1 - Niemiec, Jacek A1 - Pohl, Martin A1 - Matsumoto, Yosuke A1 - Amano, Takanobu A1 - Hoshino, Masahiro T1 - Kinetic Simulations of Nonrelativistic Perpendicular Shocks of Young Supernova Remnants BT - I. Electron Shock-surfing Acceleration JF - The astrophysical journal : an international review of spectroscopy and astronomical physics N2 - Electron injection at high Mach number nonrelativistic perpendicular shocks is studied here for parameters that are applicable to young SNR shocks. Using high-resolution large-scale two-dimensional fully kinetic particle-in-cell simulations and tracing individual particles, we in detail analyze the shock-surfing acceleration (SSA) of electrons at the leading edge of the shock foot. The central question is to what degree the process can be captured in 2D3V simulations. We find that the energy gain in SSA always arises from the electrostatic field of a Buneman wave. Electron energization is more efficient in the out-of-plane orientation of the large-scale magnetic field because both the phase speed and the amplitude of the waves are higher than for the in-plane scenario. Also, a larger number of electrons is trapped by the waves compared to the in-plane configuration. We conclude that significant modifications of the simulation parameters are needed to reach the same level of SSA efficiency as in simulations with out-of-plane magnetic field or 3D simulations. KW - acceleration of particles KW - instabilities KW - ISM: supernova remnants KW - methods: numerical KW - plasmas KW - shock waves Y1 - 2019 U6 - https://doi.org/10.3847/1538-4357/ab1b6d SN - 0004-637X SN - 1538-4357 VL - 878 IS - 1 PB - IOP Publ. Ltd. CY - Bristol ER -