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Magnetic field generation in a jet-sheath plasma via the kinetic Kelvin-Helmholtz instability

  • We have investigated the generation of magnetic fields associated with velocity shear between an unmagnetized relativistic jet and an unmagnetized sheath plasma. We have examined the strong magnetic fields generated by kinetic shear (Kelvin-Helmholtz) instabilities. Compared to the previous studies using counter-streaming performed by Alves et al. (2012), the structure of the kinetic Kelvin-Helmholtz instability (KKHI) of our jet-sheath configuration is slightly different, even for the global evolution of the strong transverse magnetic field. In our simulations the major components of growing modes are the electric field E-z, perpendicular to the flow boundary, and the magnetic field B-y, transverse to the flow direction. After the B-y component is excited, an induced electric field E-x, parallel to the flow direction, becomes significant. However, other field components remain small. We find that the structure and growth rate of KKHI with mass ratios m(i)/m(e) = 1836 and m(i)/m(e) = 20 are similar. In our simulations in the nonlinearWe have investigated the generation of magnetic fields associated with velocity shear between an unmagnetized relativistic jet and an unmagnetized sheath plasma. We have examined the strong magnetic fields generated by kinetic shear (Kelvin-Helmholtz) instabilities. Compared to the previous studies using counter-streaming performed by Alves et al. (2012), the structure of the kinetic Kelvin-Helmholtz instability (KKHI) of our jet-sheath configuration is slightly different, even for the global evolution of the strong transverse magnetic field. In our simulations the major components of growing modes are the electric field E-z, perpendicular to the flow boundary, and the magnetic field B-y, transverse to the flow direction. After the B-y component is excited, an induced electric field E-x, parallel to the flow direction, becomes significant. However, other field components remain small. We find that the structure and growth rate of KKHI with mass ratios m(i)/m(e) = 1836 and m(i)/m(e) = 20 are similar. In our simulations in the nonlinear stage is not as clear as in counter-streaming cases. The growth rate for a mildly-relativistic jet case (gamma(j) = 1.5) is larger than for a relativistic jet case (gamma(j) = 15).show moreshow less

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Metadaten
Author:K. -I. Nishikawa, P. Hardee, B. Zhang, I. Dutan, M. Medvedev, E. J. Choi, K. W. Min, J. Niemiec, Y. Mizuno, Ake Nordlund, Jacob Trier Frederiksen, H. Sol, Martin PohlORCiDGND, D. H. Hartmann
DOI:https://doi.org/10.5194/angeo-31-1535-2013
ISSN:0992-7689 (print)
Parent Title (English):Annales geophysicae
Publisher:Copernicus
Place of publication:Göttingen
Document Type:Article
Language:English
Year of first Publication:2013
Year of Completion:2013
Release Date:2017/03/26
Tag:Solar physics; astronomy (Energetic particles); astrophysics
Volume:31
Issue:9
Pagenumber:7
First Page:1535
Last Page:1541
Funder:NSF [AST-0908010, AST-0908040]; NCN [DEC-2011/01/B/ST9/03183, DEC-2012/04/A/ST9/00083]; Taiwan National Science Council [NSC 100-2112-M-007-022-MY3]; National Science Foundation [PHY05-51164]; [NASA-NNG05GK73G]; [NNX07AJ88G]; [NNX08AG83G]; [NNX08 AL39G]; [NNX09AD16G]; [NNX12AH06G]
Organizational units:Mathematisch-Naturwissenschaftliche Fakultät / Institut für Physik und Astronomie
Peer Review:Referiert
Publication Way:Open Access