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010   $a981-13-8149-6
024 7 $a10.1007/978-981-13-8149-2
035   $a(CKB)4100000008525969
035   $a(DE-He213)978-981-13-8149-2
035   $a(MiAaPQ)EBC5776241
035   $a(PPN)236523287
035   $a(EXLCZ)994100000008525969
100   $a20190502d2019      u|         0
101 0 $aeng
135   $aurnn|008mamaa
181   $ctxt$2rdacontent
182   $cc$2rdamedia
183   $acr$2rdacarrier
200 10$aEnergy Transfer and Dissipation in Plasma Turbulence             $eFrom Compressible MHD to Collisionless Plasma /$fby Yan Yang
205   $a1st ed. 2019.
210  1$aSingapore :$cSpringer Singapore :$cImprint: Springer,$d2019.
215   $a1 online resource (XIX, 134 p. 55 illus., 52 illus. in color.) 
225 1 $aSpringer Theses, Recognizing Outstanding Ph.D. Research,$x2190-5053
311   $a981-13-8148-8 
327   $aIntroduction -- Elements of Plasma Physics -- Numerical Algorithm for Compressible Magnetohydrodynamic Turbulence -- Energy Cascade in Compressible Magnetohydrodynamic Turbulence -- Energy Transfer and Dissipation in Collisionless Plasma Turbulence -- Discussion and Conclusions.
330   $aThis book revisits the long-standing puzzle of cross-scale energy transfer and dissipation in plasma turbulence and introduces new perspectives based on both magnetohydrodynamic (MHD) and Vlasov models. The classical energy cascade scenario is key in explaining the heating of corona and solar wind. By employing a high-resolution hybrid (compact finite difference & WENO) scheme, the book studies the features of compressible MHD cascade in detail, for example, in order to approximate a real plasma cascade as ?Kolmogorov-like? and to understand features that go beyond the usual simplified theories based on incompressible models. When approaching kinetic scales where plasma effects must be considered, it uses an elementary analysis of the Vlasov?Maxwell equations to help identify the channels through which energy transfer must be dissipated. In addition, it shows that the pressure?strain interaction is of great significance in producing internal energy. This analysis, in contrast to many other recent studies, does not make assumptions about wave-modes, instability or other specific mechanisms responsible for the dynamics ? the results are direct consequences of the Vlasov?Maxwell system of equations. This is an important step toward understanding dissipation in turbulent collisionless plasma in space and astrophysics.
410  0$aSpringer Theses, Recognizing Outstanding Ph.D. Research,$x2190-5053
606   $aPlasma (Ionized gases)
606   $aFluid mechanics
606   $aNumerical analysis
606   $aPlasma Physics$3https://scigraph.springernature.com/ontologies/product-market-codes/P24040
606   $aEngineering Fluid Dynamics$3https://scigraph.springernature.com/ontologies/product-market-codes/T15044
606   $aNumerical Analysis$3https://scigraph.springernature.com/ontologies/product-market-codes/M14050
615  0$aPlasma (Ionized gases)
615  0$aFluid mechanics.
615  0$aNumerical analysis.
615 14$aPlasma Physics.
615 24$aEngineering Fluid Dynamics.
615 24$aNumerical Analysis.
676   $a530.44
700   $aYang$b Yan$4aut$4http://id.loc.gov/vocabulary/relators/aut$0838755
906   $aBOOK
912   $a9910350228803321
996   $aEnergy transfer and dissipation in plasma turbulence$91873373
997   $aUNINA