On the compressibility effect in test particle acceleration by magnetohydrodynamic turbulence

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The effect of compressibility in a charged particle energization by magnetohydrodynamic (MHD) fields is studied in the context of test particle simulations. This problem is relevant to the solar wind and the solar corona due to the compressible nature of the flow in those astrophysical scenarios. We...

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Autor principal: González, C.A
Otros Autores: Dmitruk, P., Mininni, P.D, Matthaeus, W.H
Formato: Capítulo de libro
Lenguaje:Inglés
Publicado: American Institute of Physics Inc. 2016
Acceso en línea:Registro en Scopus
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100 1 |a González, C.A. 
245 1 3 |a On the compressibility effect in test particle acceleration by magnetohydrodynamic turbulence 
260 |b American Institute of Physics Inc.  |c 2016 
506 |2 openaire  |e Política editorial 
504 |a Matthaeus, W.H., Wan, M., Servidio, S., Greco, A., Osman, K.T., Oughton, S., Dmitruk, P., (2015) Philos. Trans. R. Soc., A, 373 (2041). , ISSN: 1364-503X 
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504 |a Matthaeus, W.H., Ambrosiano, J.J., Goldstein, M.L., (1984) Phys. Rev. Lett., 53, pp. 1449-1452 
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504 |a Arzner, K., Vlahos, L., Particle acceleration in multiple dissipation regions (2004) Astrophys. J. Lett., 605 (1), p. L69 
504 |a Dmitruk, P., Matthaeus, W.H., Seenu, N., (2004) Astrophys. J., 617 (1), p. 667 
504 |a Dalena, S., Rappazzo, A.F., Dmitruk, P., Greco, A., Matthaeus, W.H., (2014) Astrophys. J., 783 (2), p. 143 
504 |a Chandran, B.D.G., (2003) Astrophys. J., 599 (2), p. 1426 
504 |a Cho, J., Lazarian, A., (2006) Astrophys. J., 638 (2), p. 811 
504 |a Lynn, J.W., Quataert, E., Chandran, B.D.G., Parrish, I.J., (2013) Astrophys. J., 777 (2), p. 128 
504 |a Weidl, M.S., Jenko, F., Teaca, B., Schlickeiser, R., (2015) Astrophys. J., 811 (1), p. 8 
504 |a Teaca, B., Weidl, M.S., Jenko, F., Schlickeiser, R., (2014) Phys. Rev. e, 90 
504 |a Mininni, P.D., Rosenberg, D., Reddy, R., Pouquet, A., A hybrid MPI-OPENMP scheme for scalable parallel pseudospectral computations for fluid turbulence (2011) Parallel Comput., 37 (6-7), pp. 316-326. , ISSN: 0167-8191 
504 |a Clyne, J., Mininni, P., Norton, A., Rast, M., Interactive desktop analysis of high resolution simulations: Application to turbulent plume dynamics and current sheet formation (2007) New J. Phys., 9 (8), p. 301 
504 |a Servidio, S., Matthaeus, W.H., Shay, M.A., Dmitruk, P., Cassak, P.A., Wan, M., Statistics of magnetic reconnection in two-dimensional magnetohydrodynamic turbulence (2010) Phys. Plasmas, 17 (3) 
504 |a Dmitruk, P., Matthaeus, W.H., Test particle acceleration in three-dimensional Hall MHD turbulence (2006) J. Geophys. Res.: Space Phys., 111 A12, p. A12110. , doi: 10.1029/2006JA011988 , ISSN: 2156-2202 
504 |a Ambrosiano, J., Matthaeus, W.H., Goldstein, M.L., Plante, D., Test particle acceleration in turbulent reconnecting magnetic fields (1988) J. Geophys. Res.: Space Phys., 93 A12, pp. 14383-14400. , doi: 10.1029/JA093iA12p14383 , ISSN: 2156-2202 
504 |a Drake, J.F., Swisdak, M., Che, H., Shay, M.A., Electron acceleration from contracting magnetic islands during reconnection (2006) Nature, 443 (7111), pp. 553-556. , ISSN: 0028-0836 
520 3 |a The effect of compressibility in a charged particle energization by magnetohydrodynamic (MHD) fields is studied in the context of test particle simulations. This problem is relevant to the solar wind and the solar corona due to the compressible nature of the flow in those astrophysical scenarios. We consider turbulent electromagnetic fields obtained from direct numerical simulations of the MHD equations with a strong background magnetic field. In order to explore the flow compressibility effect over the particle dynamics, we performed different numerical experiments: an incompressible case and two weak compressible cases with Mach number M = 0.1 and M = 0.25. We analyze the behavior of protons and electrons in those turbulent fields, which are well known to form aligned current sheets in the direction of the guide magnetic field. What we call protons and electrons are test particles with scales comparable to (for protons) and much smaller than (for electrons) the dissipative scale of MHD turbulence, maintaining the correct mass ratio m e / m i. For these test particles, we show that compressibility enhances the efficiency of proton acceleration, and that the energization is caused by perpendicular electric fields generated between currents sheets. On the other hand, electrons remain magnetized and display an almost adiabatic motion, with no effect of compressibility observed. Another set of numerical experiments takes into account two fluid modifications, namely, electric field due to Hall effect and electron pressure gradient. We show that the electron pressure has an important contribution to electron acceleration allowing highly parallel energization. In contrast, no significant effect of these additional terms is observed for the protons. © 2016 Author(s).  |l eng 
536 |a Detalles de la financiación: Secretaría de Ciencia y Técnica, Universidad de Buenos Aires, PICT 2011-1529, 2011-1626, 2011-0454, 20020110200359, 20020100100315 
536 |a Detalles de la financiación: NNX14AI63G, NNX15AB88G 
536 |a Detalles de la financiación: Southwest Research Institute, D99031L 
536 |a Detalles de la financiación: The authors thank an anonymous reviewer for useful comments that resulted in the study of electron pressure effects. C.A.G., P.D., and P.D.M. acknowledge support from Grant UBACyT Nos. 20020110200359 and 20020100100315, and from Grant Nos. PICT 2011-1529, 2011-1626, and 2011-0454. W.H.M. was partially supported by NASA LWS-TRT Grant NNX15AB88G, Grand Challenge Research Grant NNX14AI63G, and the Solar Probe Plus mission through the Southwest Research Institute ISIS project D99031L. 
593 |a Departamento de Física, Facultad de Ciencias Exactas y Naturales, Universidad de Buenos Aires, IFIBA, CONICET, Ciudad Universitaria, Buenos Aires, 1428, Argentina 
593 |a Bartol Research Institute, Department of Physics and Astronomy, University of Delaware, Newark, DE 19716, United States 
690 1 0 |a ACCELERATION 
690 1 0 |a CHARGED PARTICLES 
690 1 0 |a COMPRESSIBILITY 
690 1 0 |a ELECTRIC FIELDS 
690 1 0 |a ELECTROMAGNETIC FIELDS 
690 1 0 |a ELECTRONS 
690 1 0 |a INCOMPRESSIBLE FLOW 
690 1 0 |a KINETIC THEORY 
690 1 0 |a MAGNETIC FIELDS 
690 1 0 |a TURBULENCE 
690 1 0 |a COMPRESSIBILITY EFFECTS 
690 1 0 |a ELECTRON ACCELERATION 
690 1 0 |a ELECTRON PRESSURES 
690 1 0 |a GUIDE MAGNETIC FIELD 
690 1 0 |a MAGNETOHYDRODYNAMIC TURBULENCE 
690 1 0 |a NUMERICAL EXPERIMENTS 
690 1 0 |a PARTICLE DYNAMICS 
690 1 0 |a PROTON ACCELERATION 
690 1 0 |a MAGNETOHYDRODYNAMICS 
700 1 |a Dmitruk, P. 
700 1 |a Mininni, P.D. 
700 1 |a Matthaeus, W.H. 
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