Dataset.

3D PIC Simulations for relativistic jets with a toroidal magnetic field [Dataset]

Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/359865
Digital.CSIC. Repositorio Institucional del CSIC
  • Meli, Athina
  • Nishikawa, Kenichi
  • Köhn, Christoph
  • Duţan, Iona
  • Mizuno, Yosuke
  • Kobzar, Oleh
  • MacDonald, Nicholas
  • Gómez, José L.
  • Hirotani, Kouichi
Supplementary PIC simulation movies for the MNRAS article titled ''3D PIC Simulations for Relativistic Jets with a Toroidal Magnetic Field'', by Meli, Nishikawa, Kohn, et al, With funding from the Spanish government through the "Severo Ochoa Centre of Excellence" accreditation (CEX2021-001131-S)., Peer reviewed
 

DOI: http://hdl.handle.net/10261/359865
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/359865

HANDLE: http://hdl.handle.net/10261/359865
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/359865
 
Ver en: http://hdl.handle.net/10261/359865
Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/359865

Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/307547
Artículo científico (article). 2023

3D PIC SIMULATIONS FOR RELATIVISTIC JETS WITH A TOROIDAL MAGNETIC FIELD

Digital.CSIC. Repositorio Institucional del CSIC
  • Meli, Athina
  • Nishikawa, Kenichi
  • Köhn, Christoph
  • Duţan, Ioana
  • Mizuno, Yosuke
  • Kobzar, Oleh
  • MacDonald, Nicholas
  • Gómez, José L.
  • Hirotani, Kouichi
We have investigated how kinetic instabilities such as the Weibel instability (WI), the mushroom instability (MI), and the kinetic Kelvin–Helmholtz instability (kKHI) are excited in jets without and with a toroidal magnetic field, and how such instabilities contribute to particle acceleration. In this work, we use a new jet injection scheme, where an electric current is self-consistently generated at the jet orifice by the jet particles, which produce the toroidal magnetic field. We perform five different simulations for a sufficiently long time to examine the non-linear effects of the jet evolution. We inject unmagnetized e± and e−– p+ (mp/me = 1836), as well as magnetized e± and e−– i+ (mi/me = 4) jets with a top-hat jet density profile into an unmagnetized ambient plasmas of the same species. We show that WI, MI, and kKHI excited at the linear stage, generate a non-oscillatory x-component of the electric field accelerating, and decelerating electrons. We find that the two different jet compositions (e± and e−– i+) display different instability modes, respectively. Moreover, the magnetic field in the non-linear stage generated by different instabilities is dissipated and reorganized into new topologies. A 3D magnetic field topology depiction indicates possible reconnection sites in the non-linear stage, where the particles are significantly accelerated by the dissipation of the magnetic field associated to a possible reconnection event. © 2022 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society., This work was supported by the National Aeronautics and Space Administration (NASA)-NNX12AH06G, NNX13AP-21G, and NNX13AP14G grants. Recent work was also provided by the NASA through Chandra Award Number GO7-18118X (PI: Ming Sun at UAH) issued by the Chandra X-ray Center, which is operated by the SAO for and on behalf of the NASA under contract NAS8-03060. The simulations presented in this report have been performed by Frontera supercomputer at the Texas Advanced Computing Center under the AST21038: Computational Study of Astrophysical Plasmas, and also provided by the NASA through by the grant: Nature Of Hard X-rays From A TeV-detected RadioGalaxy (PI: Ka Wah Wong at SUNY Brockport) issued by the NuSTAR Guest Observer Cycle 6 2019. Y.M. is supported by the ERC Synergy Grant ‘BlackHoleCam: Imaging the Event Horizon of Black Holes’ (Grant No. 610058). The work of I.D. has been supported by the NUCLEU project. Simulations were performed using Pleiades and Endeavor facilities at NASA Advanced Supercomputing (NAS: s2004), using Comet at The San Diego Supercomputer Center (SDSC), and Bridges at the Pittsburgh Supercomputing Center, which are supported by the National Science Foundation (NSF). JLG acknowledges the support of the Spanish Ministerio de Economía y Competitividad (grants AYA2016-80889-P, PID2019-108995GB-C21), the Consejería de Economía, Conocimiento, Empresas y Universidad, Junta de Andalucía (grant P18-FR-1769), the Consejo Superior de Investigaciones Científicas (grant 2019AEP112), and the State Agency for Research of the Spanish MCIU through the Center of Excellence Severo Ochoa award for the Instituto de Astrofísica de Andalucía (SEV-2017-0709)., With funding from the Spanish government through the "Severo Ochoa Centre of Excellence" accreditation (CEX2021-001131-S)., Peer reviewed




Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/358149
Capítulo o parte de un libro (bookPart). 2024

3D PIC SIMULATIONS FOR RELATIVISTIC JETS WITH A TOROIDAL MAGNETIC FIELD

Digital.CSIC. Repositorio Institucional del CSIC
  • Nishikawa, Kenichi
  • Meli, Athina
  • Köhn, Christoph
  • Duţan, Ioana
  • Mizuno, Yosuke
  • Kobzar, Oleh
  • MacDonald, Nicholas
  • Gómez, José L.
  • Hirotani, Kouichi
Part of Proceedings of the International Astronomical Union (IAU S375) pp. 44-48, Particle-in-Cell simulations can provide a possible answer to an important key issue for astrophysical plasma jets; namely on how a toroidal magnetic field affects the evolution of pair and electron-ion jets. We show that Weibel, mushroom, and kinetic Kelvin-Helmhotz instabilities excited at the linear stage, generate a quasi-steady x-component of the electric field which accelerates and decelerates electrons. We observe significant differences in the structure of the strong electromagnetic fields that are driven by the kinetic instabilities with the pair jet. We find that the two different jet compositions (e± and e- - i+) generate different instability modes respectively. Moreover, the magnetic field in the non-linear stage generated by different instabilities is dissipated and reorganized into new topologies. A 3D magnetic field topology depiction indicates possible reconnection sites in the non-linear stage where the particles are significantly accelerated by the dissipation of the magnetic field associated to a possible reconnection manifestation. © The Author(s), 2023. Published by Cambridge University Press on behalf of International Astronomical Union




Digital.CSIC. Repositorio Institucional del CSIC
oai:digital.csic.es:10261/359865
Dataset. 2023

3D PIC SIMULATIONS FOR RELATIVISTIC JETS WITH A TOROIDAL MAGNETIC FIELD [DATASET]

Digital.CSIC. Repositorio Institucional del CSIC
  • Meli, Athina
  • Nishikawa, Kenichi
  • Köhn, Christoph
  • Duţan, Iona
  • Mizuno, Yosuke
  • Kobzar, Oleh
  • MacDonald, Nicholas
  • Gómez, José L.
  • Hirotani, Kouichi
Supplementary PIC simulation movies for the MNRAS article titled ''3D PIC Simulations for Relativistic Jets with a Toroidal Magnetic Field'', by Meli, Nishikawa, Kohn, et al, With funding from the Spanish government through the "Severo Ochoa Centre of Excellence" accreditation (CEX2021-001131-S)., Peer reviewed




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