000			03476nam a2200469 i 4500
001			0000175772
005			20171002064013.0
006			m o d
007			cr cn|||||||||
008			130502t20142014njua ob 001 0 eng|d
020			_z9780691141725 (hardback)
020			_z9780691141732 (paperback)
020			_a9781400848904 (e-book)
035			_a(CaPaEBR)ebr10783690
035			_a(OCoLC)864358299
040			_aCaPaEBR _beng _erda _epn _cCaPaEBR
050	1	4	_aQB462.3 _b.G53 2014eb
082	0	4	_a523.4 _223
100	1		_aGlatzmaier, Gary A., _d1949-
245	1	0	_aIntroduction to modeling convection in planets and stars : _bmagnetic field, density stratification, rotation / _cGary A. Glatzmaier.
264		1	_aPrinceton : _bPrinceton University Press, _c[2014]
264		4	_c©2014
300			_a1 online resource (342 pages) : _billustrations.
336			_atext _2rdacontent
337			_acomputer _2rdamedia
338			_aonline resource _2rdacarrier
440		0	_aPrinceton series in astrophysics
504			_aIncludes bibliographical references and index.
505	0		_apart I. The fundamentals -- part II. Additional numerical methods -- part III. Additional physics.
520			_a"This book provides readers with the skills they need to write computer codes that simulate convection, internal gravity waves, and magnetic field generation in the interiors and atmospheres of rotating planets and stars. Using a teaching method perfected in the classroom, Gary Glatzmaier begins by offering a step-by-step guide on how to design codes for simulating nonlinear time-dependent thermal convection in a two-dimensional box using Fourier expansions in the horizontal direction and finite differences in the vertical direction. He then describes how to implement more efficient and accurate numerical methods and more realistic geometries in two and three dimensions. In the third part of the book, Glatzmaier demonstrates how to incorporate more sophisticated physics, including the effects of magnetic field, density stratification, and rotation.Featuring numerous exercises throughout, this is an ideal textbook for students and an essential resource for researchers. Describes how to create codes that simulate the internal dynamics of planets and stars Builds on basic concepts and simple methods Shows how to improve the efficiency and accuracy of the numerical methods Describes more relevant geometries and boundary conditions Demonstrates how to incorporate more sophisticated physics "-- _cProvided by publisher.
588			_aDescription based on print version record.
590			_aElectronic reproduction. Palo Alto, Calif. : ebrary, 2013. Available via World Wide Web. Access may be limited to ebrary affiliated libraries.
650		0	_aConvection (Astrophysics) _xComputer simulation.
650		0	_aConvection (Astrophysics) _xMathematical models.
650		0	_aPlanets _xAtmospheres.
650		0	_aStars _xAtmospheres.
655		0	_aElectronic books.
776	0	8	_iPrint version: _aGlatzmaier, Gary A. _tIntroduction to modeling convection in planets and stars : magnetic field, density stratification, rotation. _dPrinceton : Princeton University Press, [2014] _hxiii, 311 pages _kPrinceton series in astrophysics _z9780691141732 _w(DLC) 2013010051
797	2		_aebrary.
856	4	0	_uhttp://site.ebrary.com/lib/daystar/Doc?id=10783690 _zAn electronic book accessible through the World Wide Web; click to view
908			_a170314
942	0	0	_cEB
999			_c164913 _d164913