LEADER 05966nam 22007335 450 001 9910254122303321 005 20200702083025.0 010 $a3-662-48310-6 024 7 $a10.1007/978-3-662-48310-7 035 $a(CKB)3710000000466564 035 $a(EBL)4178936 035 $a(SSID)ssj0001546818 035 $a(PQKBManifestationID)16141441 035 $a(PQKBTitleCode)TC0001546818 035 $a(PQKBWorkID)14795992 035 $a(PQKB)11309777 035 $a(DE-He213)978-3-662-48310-7 035 $a(MiAaPQ)EBC4178936 035 $a(PPN)188462236 035 $a(EXLCZ)993710000000466564 100 $a20150821d2016 u| 0 101 0 $aeng 135 $aur|n|---||||| 181 $ctxt 182 $cc 183 $acr 200 10$aMagnetic Cloud Boundary Layers and Magnetic Reconnection$b[electronic resource] /$fby Yi Wang 205 $a1st ed. 2016. 210 1$aBerlin, Heidelberg :$cSpringer Berlin Heidelberg :$cImprint: Springer,$d2016. 215 $a1 online resource (81 p.) 225 1 $aSpringer Theses, Recognizing Outstanding Ph.D. Research,$x2190-5053 300 $aDescription based upon print version of record. 311 $a3-662-48309-2 320 $aIncludes bibliographical references at the end of each chapters. 327 $aSupervisor's Foreword; Acknowledgments; Contents; 1 Introduction; 1.1 Magnetic Reconnection; 1.1.1 Sweet-Parker Reconnection; 1.1.2 Hall Reconnection; 1.1.3 Petschek Reconnection; 1.1.4 Open Questions; 1.2 Particle Acceleration in Magnetic Reconnection; 1.2.1 Acceleration Region and Acceleration Process; 1.2.2 Acceleration Mechanism; 1.2.3 Open Questions; 1.3 Magnetic Cloud Boundary Layer; 1.3.1 The Identification of MC Boundary; 1.3.2 Properties of the BL; 1.3.3 Open Questions; 1.4 Magnetic Reconnection in the Solar Wind; 1.4.1 Structure of the Reconnection Exhaust 327 $a1.4.2 Physical Properties of Magnetic Reconnections in the Solar Wind1.4.3 Open Questions; References; 2 Magnetic Reconnection and the Associated Energetic Particles in the Boundary Layer; 2.1 Introduction; 2.2 Analyzing Methods; 2.2.1 LMN Coordinate; 2.2.2 Walen Relation; 2.3 Magnetic Reconnection in the BL; 2.4 Energetic Particles Associated with Magnetic Reconnection; 2.5 Discussion and Conclusion; References; 3 The Acceleration of Energetic Particles in Magnetic Reconnection; 3.1 Introduction; 3.2 Background Description of Numerical Simulations 327 $a3.2.1 Different Methods of Numerical Simulations3.2.2 GEM Magnetic Reconnection Challenge; 3.3 Simulation Results; 3.3.1 Interplanetary Magnetic Reconnection Driven by MC; 3.3.2 Acceleration of Energetic Electrons; 3.4 Discussion and Summary; References; 4 Proton and Electron Flux Variations in the Magnetic Cloud Boundary Layers; 4.1 Introduction; 4.2 The Velocity Distribution Function; 4.2.1 Definition of the Velocity Distribution Function; 4.2.2 The Moments of the Velocity Distribution Function; 4.2.3 Electron Velocity Distribution Function in Solar Wind; 4.3 Data Set Description 327 $a4.3.1 Instruments and Data4.3.2 Event Selection; 4.4 Statistical Results; 4.5 Explanations for the Flux Variations at Different Energy Bands; 4.5.1 The Core Electrons; 4.5.2 The Suprathermal Electrons; 4.5.3 Energetic Electrons; 4.5.4 Protons; 4.6 Discussion and Summary; References; 5 The Criterion of Magnetic Reconnection in the Solar Wind; 5.1 Introduction; 5.2 Event Selection; 5.2.1 The Reconnection Exhaust; 5.2.2 The MC-Driven Shock; 5.3 Statistical Results; 5.4 Explanations for the Flux Variations in Different Events; 5.4.1 The Magnetic Cloud Boundary Layer and Reconnection Exhaust 327 $a5.4.2 The MC-Driven Shock5.5 Discussion and Summary; References; 6 Summary and Outlook; References 330 $aThis thesis focuses on magnetic reconnection processes in the boundary layer of the interplanetary magnetic cloud. Magnetic reconnection is an important and frontier topic in the realm of physics. Various physical phenomena can be observed during the reconnection process but lots of them are not fully understood. This thesis provides the first observational evidence of energetic electrons associated with magnetic reconnection in the solar wind and discusses the particle acceleration problems. In addition, after analyzing the particle flux variations in Magnetic Cloud Boundary Layer, the thesis proposes a possible new criterion for the identification of magnetic reconnection in the solar wind. These tantalizing results could be particular clues to understand the dynamical problems in magnetic reconnection processes. 410 0$aSpringer Theses, Recognizing Outstanding Ph.D. Research,$x2190-5053 606 $aGeophysics 606 $aSpace sciences 606 $aPlasma (Ionized gases) 606 $aGeophysics/Geodesy$3https://scigraph.springernature.com/ontologies/product-market-codes/G18009 606 $aGeophysics and Environmental Physics$3https://scigraph.springernature.com/ontologies/product-market-codes/P32000 606 $aSpace Sciences (including Extraterrestrial Physics, Space Exploration and Astronautics)$3https://scigraph.springernature.com/ontologies/product-market-codes/P22030 606 $aPlasma Physics$3https://scigraph.springernature.com/ontologies/product-market-codes/P24040 615 0$aGeophysics. 615 0$aSpace sciences. 615 0$aPlasma (Ionized gases). 615 14$aGeophysics/Geodesy. 615 24$aGeophysics and Environmental Physics. 615 24$aSpace Sciences (including Extraterrestrial Physics, Space Exploration and Astronautics). 615 24$aPlasma Physics. 676 $a551.5153 700 $aWang$b Yi$4aut$4http://id.loc.gov/vocabulary/relators/aut$0927188 801 0$bMiAaPQ 801 1$bMiAaPQ 801 2$bMiAaPQ 906 $aBOOK 912 $a9910254122303321 996 $aMagnetic Cloud Boundary Layers and Magnetic Reconnection$92508104 997 $aUNINA