000			03217nam a22003855i 4500
001			288124
003			MX-SnUAN
005			20160429154616.0
007			cr nn 008mamaa
008			150903s2013 xxu| o |||| 0|eng d
020			_a9781461460992 _99781461460992
024	7		_a10.1007/9781461460992 _2doi
035			_avtls000341819
039		9	_a201509030340 _bVLOAD _c201405050234 _dVLOAD _y201402061109 _zstaff
040			_aMX-SnUAN _bspa _cMX-SnUAN _erda
050		4	_aQB495-500.269
100	1		_aBalogh, André. _eautor _9303831
245	1	0	_aPhysics of Collisionless Shocks : _bSpace Plasma Shock Waves / _cby André Balogh, Rudolf A. Treumann.
264		1	_aNew York, NY : _bSpringer New York : _bImprint: Springer, _c2013.
300			_axii, 500 páginas 170 ilustraciones, 38 ilustraciones en color. _brecurso en línea.
336			_atexto _btxt _2rdacontent
337			_acomputadora _bc _2rdamedia
338			_arecurso en línea _bcr _2rdacarrier
347			_aarchivo de texto _bPDF _2rda
490	0		_aISSI Scientific Report Series ; _v12
500			_aSpringer eBooks
505	0		_aPart I -- The Shock Problem -- Equations and Models -- Subcritical Shocks -- Quasi-Perpendicular Supercritical Shocks -- Quasi-Parallel Supercritical Shocks -- Particle Acceleration -- Final Remarks -- Part II -- Introduction.- Planetary Bow Shocks.- The Heliospheric Termination Shock.
520			_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.
590			_aPara consulta fuera de la UANL se requiere clave de acceso remoto.
700	1		_aTreumann, Rudolf A. _eautor _9317707
710	2		_aSpringerLink (Servicio en línea) _9299170
776	0	8	_iEdición impresa: _z9781461460985
856	4	0	_uhttp://remoto.dgb.uanl.mx/login?url=http://dx.doi.org/10.1007/978-1-4614-6099-2 _zConectar a Springer E-Books (Para consulta externa se requiere previa autentificación en Biblioteca Digital UANL)
942			_c14
999			_c288124 _d288124