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001			301933
003			MX-SnUAN
005			20160429155728.0
007			cr nn 008mamaa
008			150903s2010 gw | o |||| 0|eng d
020			_a9783642130304 _99783642130304
024	7		_a10.1007/9783642130304 _2doi
035			_avtls000355036
039		9	_a201509030949 _bVLOAD _c201405060344 _dVLOAD _y201402191033 _zstaff
040			_aMX-SnUAN _bspa _cMX-SnUAN _erda
050		4	_aQB460-466
100	1		_aSmeyers, Paul. _eautor _9309579
245	1	0	_aLinear Isentropic Oscillations of Stars : _bTheoretical Foundations / _cby Paul Smeyers, Tim Van Hoolst.
264		1	_aBerlin, Heidelberg : _bSpringer Berlin Heidelberg : _bImprint: Springer, _c2010.
300			_axiv, 473 páginas _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		_aAstrophysics and Space Science Library, _x0067-0057 ; _v371
500			_aSpringer eBooks
505	0		_aBasic Concepts -- The Equations Governing Linear Perturbations in a Quasi-Static Star -- Deviations from the Hydrostatic and Thermal Equilibrium in a Quasi-Static Star -- Eigenvalue Problem of the Linear, Isentropic Normal Modes in a Quasi-Static Star -- Spheroidal and Toroidal Normal Modes -- Determination of Spheroidal Normal Modes: Mathematical Aspects -- The Eulerian Perturbation of the Gravitational Potential -- The Variational Principle of Hamilton -- Radial Propagation of Waves -- Classification of the Spheroidal Normal Modes -- Classification of the Spheroidal Normal Modes (continued) -- Completeness of the Linear, Isentropic Normal Modes -- N 2(r) Nowhere Negative as Condition for Non-Radial Modes with Real Eigenfrequencies -- Asymptotic Representation of Low-Degree, Higher-Order p-Modes -- Asymptotic Representation of Low-Degree and Intermediate-Degree p-Modes -- Asymptotic Representation of Low-Degree, Higher-Order g +-Modes in Stars Containing a Convective Core -- Asymptotic Representation of Low-Degree, Higher-Order g +-Modes in Stars Consisting of a Radiative Core and a Convective Envelope -- High-Degree, Low-Order Modes -- Period Changes in a Rapidly Evolving Pulsating Star.
520			_aThe study of stellar oscillations is the preeminent way to investigate the stability of stars and to interpret their variability. The theory of the linear, isentropic oscillations of isolated gaseous stars, and thus of compressible spherically symmetric equilibrium configurations, has largely been developed from the viewpoint of the hypothesis of the physical radial pulsations of stars. Written for doctoral students and researchers, this monograph aims to provide a systematic and consistent survey of the fundamentals of the theory of free, linear, isentropic oscillations in spherically symmetric, gaseous equilibrium stars. The first part of the book presents basic concepts and equations, the distinction between spheroidal and toroidal normal modes, the solution of Poisson’s differential equation for the perturbation of the gravitational potential, and Hamilton’s variational principle. The second part is devoted to the possible existence of waves propagating in the radial direction, the origin and classification of normal modes, the completeness of the normal modes, and the relation between the local stability with respect to convection and the global stability of a star. The third part deals with asymptotic representations of normal modes and with slow period changes in rapidly evolving pulsating stars.
590			_aPara consulta fuera de la UANL se requiere clave de acceso remoto.
700	1		_aVan Hoolst, Tim. _eautor _9339994
710	2		_aSpringerLink (Servicio en línea) _9299170
776	0	8	_iEdición impresa: _z9783642130298
856	4	0	_uhttp://remoto.dgb.uanl.mx/login?url=http://dx.doi.org/10.1007/978-3-642-13030-4 _zConectar a Springer E-Books (Para consulta externa se requiere previa autentificación en Biblioteca Digital UANL)
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999			_c301933 _d301933