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Autor(en): 
  • Rudolf A. Treumann
  • André Balogh
  • Physics of Collisionless Shocks: Space Plasma Shock Waves 
     

    (Buch)
    Dieser Artikel gilt, aufgrund seiner Grösse, beim Versand als 3 Artikel!


    Übersicht

    Auf mobile öffnen
     
    Lieferstatus:   Auf Bestellung (Lieferzeit unbekannt)
    Veröffentlichung:  Juni 2015  
    Genre:  Naturwissensch., Medizin, Technik 
     
    Astrophysics / Astrophysics and Astroparticles / B / Physics and Astronomy / Plasma (Ionized gases) / Plasma Physics / Space Physics / Space sciences
    ISBN:  9781489990648 
    EAN-Code: 
    9781489990648 
    Verlag:  Springer Nature EN 
    Einband:  Kartoniert  
    Sprache:  English  
    Serie:  #12 - ISSI Scientific Report Series  
    Dimensionen:  H 235 mm / B 155 mm / D  
    Gewicht:  7664 gr 
    Seiten:  500 
    Illustration:  XII, 500 p. 
    Zus. Info:  Previously published in hardcover 
    Bewertung: Titel bewerten / Meinung schreiben
    Inhalt:
    The 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 subcritical shocks which dissipate flow energy by generating anomalous resistance or viscosity. 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.
      
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