000			02923nam a22004098i 4500
001			CR9780511667459
003			UkCbUP
005			20200124160233.0
006			m|||||o||d||||||||
007			cr||||||||||||
008			091222s2014||||enk o ||1 0|eng|d
020			_a9780511667459 (ebook)
020			_z9780521190558 (hardback)
040			_aUkCbUP _beng _erda _cUkCbUP
050	0	0	_aQC754.2.M3 _bW45 2014
082	0	0	_a538/.7 _223
100	1		_aWeiss, N. O. _q(Nigel Oscar), _eauthor.
245	1	0	_aMagnetoconvection / _cN.O. Weiss, University of Cambridge, M.R.E. Proctor, University of Cambridge.
264		1	_aCambridge : _bCambridge University Press, _c2014.
300			_a1 online resource (xi, 397 pages) : _bdigital, PDF file(s).
336			_atext _btxt _2rdacontent
337			_acomputer _bc _2rdamedia
338			_aonline resource _bcr _2rdacarrier
490	1		_aCambridge monographs on mechanics
500			_aTitle from publisher's bibliographic system (viewed on 05 Oct 2015).
505	0		_aPreface -- 1. Introduction -- 2. Basic MHD -- 3. Linearized Boussinesq magnetoconvection -- 4. The nonlinear regime -- 5. 2D Boussinesq magnetoconvection -- 6. 3D Boussinesq magnetoconvection -- 7. Magnetoconvection, rotation and the dynamo -- 8. Compressible magnetoconvection -- 9. Solar and stellar magnetic fields -- Appendix A. The Boussinesq and anelastic approximations -- Appendix B. Chaotic systems -- Appendix C. Double-diffusive convection -- Appendix D. Magnetic buoyancy and the magneto-Boussinesq approximation -- References -- Index.
520			_aThe last thirty years have seen great leaps forward in the subject of magnetoconvection. Computational techniques can now explain exotic nonlinear behaviour, transition to chaos and the formation of structures that can be observed on the surface of the Sun. Here, two leading experts present the current state of knowledge of the subject. They provide a mathematical and numerical treatment of the interactions between electrically conducting fluids and magnetic fields that lead to the complex structures and rich behaviour observed on the Sun and other stars, as well as in the interiors of planets like the Earth. The authors' combined analytical and computational approach provides a model for the study of a wide range of related problems. The discussion includes bifurcation theory, chaotic behaviour, pattern formation in two and three dimensions, and applications to geomagnetism and to the properties of sunspots and other features at the solar surface.
650		0	_aMagnetic fields.
650		0	_aSolar magnetic fields.
650		0	_aGeomagnetism.
650		0	_aMagnetohydrodynamics.
650		0	_aRelativistic fluid dynamics.
700	1		_aProctor, M. R. E., _eauthor.
776	0	8	_iPrint version: _z9780521190558
830		0	_aCambridge monographs on mechanics.
856	4	0	_uhttps://doi.org/10.1017/CBO9780511667459
999			_c517828 _d517826