LEADER 03271nam 2200637 a 450 001 9910437979703321 005 20200520144314.0 010 $a1-4614-6099-9 010 $a1-283-94573-8 024 7 $a10.1007/978-1-4614-6099-2 035 $a(CKB)2670000000530118 035 $a(EBL)1082081 035 $a(OCoLC)823728906 035 $a(SSID)ssj0000870763 035 $a(PQKBManifestationID)11474730 035 $a(PQKBTitleCode)TC0000870763 035 $a(PQKBWorkID)10819996 035 $a(PQKB)11544954 035 $a(DE-He213)978-1-4614-6099-2 035 $a(MiAaPQ)EBC1082081 035 $a(PPN)168304716 035 $a(EXLCZ)992670000000530118 100 $a20121221d2013 uy 0 101 0 $aeng 135 $aur|n|---||||| 181 $ctxt 182 $cc 183 $acr 200 10$aPhysics of collisionless shocks $espace plasma shock waves /$fAndre Balogh, Rudolf A. Treumann 205 $a1st ed. 2013. 210 $aNew York $cSpringer$d2013 215 $a1 online resource (501 p.) 225 0 $aISSI scientific report series ;$vv. 12 300 $aDescription based upon print version of record. 311 $a1-4614-6098-0 311 $a1-4899-9064-X 320 $aIncludes bibliographical references and index. 327 $apt. 1. Collisionless shock theory -- pt. 2. Applications : two kinds of collisionless shocks in the heliosphere. 330 $aThe present book provides a contemporary systematic treatment of shock waves in high-temperature collisionless plasmas as are encountered in near Earth space and in Astrophysics. It consists of two parts. Part I develops the complete theory of shocks in dilute hot plasmas under the assumption of absence of collisions among the charged particles when the interaction is mediated solely by the self-consistent electromagnetic fields. Such shocks are naturally magnetised implying that the magnetic field plays an important role in their evolution and dynamics. This part treats both subcritical shocks, which dissipate flow energy by generating anomalous resistance or viscosity, and supercritical shocks. The main emphasis is, however, on super-critical shocks where the anomalous dissipation is insufficient to retard the upstream flow. These shocks, depending on the direction of the upstream magnetic field, are distinguished as quasi-perpendicular and quasi-parallel shocks which exhibit different behaviours, reflecting particles back upstream and generating high electromagnetic wave intensities. Particle acceleration and turbulence at such shocks become possible and important. Part II treats planetary bow shocks and the famous Heliospheric Termination shock as examples of two applications of the theory developed in Part I. 410 0$aISSI Scientific Report Series 606 $aPlasma waves 606 $aShock waves 606 $aSpace plasmas 615 0$aPlasma waves. 615 0$aShock waves. 615 0$aSpace plasmas. 676 $a530.442 700 $aBalogh$b Andre$0858470 701 $aTreumann$b Rudolf A$0294050 801 0$bMiAaPQ 801 1$bMiAaPQ 801 2$bMiAaPQ 906 $aBOOK 912 $a9910437979703321 996 $aPhysics of collisionless shocks$94191322 997 $aUNINA