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000856302 019__ $$a1055430138$$a1055699838$$a1060595790
000856302 020__ $$a9783319982588$$q(electronic book)
000856302 020__ $$a3319982583$$q(electronic book)
000856302 020__ $$z9783319982571
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000856302 0247_ $$a10.1007/978-3-319-98258-8$$2doi
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000856302 050_4 $$aQB843.N4
000856302 08204 $$a523.8/874$$223
000856302 1001_ $$aPnigouras, Pantelis,$$eauthor.
000856302 24510 $$aSaturation of the f-mode instability in neutron stars /$$cPantelis Pnigouras.
000856302 264_1 $$aCham, Switzerland :$$bSpringer,$$c2018.
000856302 300__ $$a1 online resource.
000856302 336__ $$atext$$btxt$$2rdacontent
000856302 337__ $$acomputer$$bc$$2rdamedia
000856302 338__ $$aonline resource$$bcr$$2rdacarrier
000856302 347__ $$atext file$$bPDF$$2rda
000856302 4901_ $$aSpringer theses
000856302 500__ $$a"Doctoral thesis accepted by the Eberhard-Karls University of Tübingen, Tübingen, Germany."
000856302 504__ $$aIncludes bibliographical references.
000856302 5050_ $$aIntro; Supervisor's Foreword; References; Preface; References; Acknowledgements; Contents; List of Figures; List of Tables; 1 Introduction; 1.1 Prologue: Music of the Spheres; 1.2 Asteroseismology; 1.3 Neutron Stars Inside Out; 1.4 Odes from Modes; References; 2 The Oscillation Modes: Linear Perturbation Scheme; 2.1 The Fluid Equations; 2.2 Linear Perturbation Formalism; 2.3 Nonrotating Stars; 2.3.1 *Separation of Variables; 2.3.2 *Boundary Conditions; 2.3.3 *Dimensionless Formulation; 2.3.4 *The Cowling Approximation; 2.3.5 *Mode Trapping; 2.3.6 *A Trivial Solution.
000856302 5058_ $$a2.3.7 Mode Orthogonality, Decomposition, and Energy2.4 Classes of Modes; 2.4.1 Polar Modes; 2.4.2 Axial Modes; 2.4.3 Hybrid Modes; 2.5 *The Homogeneous Model; 2.6 Rotating Stars; 2.6.1 Mode Orthogonality, Decomposition, and Energy; 2.6.2 The Slow-Rotation Approximation; References; 3 The f-mode Instability; 3.1 *Figures of Equilibrium; 3.2 The Kepler Limit; 3.3 *Maclaurin, Jacobi, or Dedekind?; 3.4 *A Mechanical Example; 3.5 The CFS Instability; 3.6 The Instability Window; References; 4 Mode Coupling: Quadratic Perturbation Scheme; 4.1 Quadratic Perturbation Formalism.
000856302 5058_ $$a4.2 Resonant Mode Coupling4.2.1 Coupled Triplet Equations of Motion; 4.2.2 *The Multiscale Method; 4.2.3 Coupling Selection Rules; 4.2.4 Mode Normalisation; 4.3 Parametric Resonance Instability; 4.4 Saturation; 4.4.1 Stability Conditions; 4.4.2 Possible Evolutions; 4.4.3 *Frequency Synchronisation; References; 5 Results; 5.1 Setup; 5.1.1 *Eigenfrequencies and Eigenfunctions; 5.1.2 *Growth/Damping Rates; 5.1.3 *Couplings; 5.1.4 Saturation; 5.2 Approximate Relations for the Parametric Instability Threshold; 5.3 Typical Neutron Stars; 5.3.1 Instability Evolution; 5.3.2 Models; 5.3.3 Discussion.
000856302 5058_ $$a5.4 Supramassive Neutron Stars5.4.1 Instability Evolution; 5.4.2 Models; 5.4.3 Discussion; 5.5 Stochastic Background; 5.6 *Comparison with r-modes; References; 6 Final Remarks; 6.1 Summary and Conclusions; 6.2 Epilogue: Notes on the Cosmic Staff; References; Appendix A Polytropic Stars; A.1 Nonrotating Polytropes; A.2 Rotating Polytropes; Appendix B Polar Mode Rotational Corrections; B.1 First-Order Corrections; B.2 Second-Order Corrections; B.2.1 Generic Formulation; B.2.2 Application to Polytropes; Appendix C Polar Mode Growth/Damping Rates; C.1 Gravitational Waves; C.2 Shear Viscosity.
000856302 5058_ $$aC.3 Bulk ViscosityC. 4 Mode Energy; Appendix D Equations of Motion; D.1 Equation of Motion for Quadratic Perturbations; D.2 Amplitude Equation of Motion; Appendix E Polar Mode Coupling Coefficient; E.1 Parametrised Form; E.2 Angular Part; E.3 Radial Part; Appendix F Parametrically Unstable Mode Triplet; F.1 Parametric Instability Threshold; F.2 Equilibrium Solution; F.3 Linear Stability Analysis; Appendix G Coupling Spectrum.
000856302 506__ $$aAccess limited to authorized users.
000856302 520__ $$aThis book presents a study of the saturation of unstable f-modes (fundamental modes) due to low-order nonlinear mode coupling. Since their theoretical prediction in 1934, neutron stars have remained among the most challenging objects in the Universe. Gravitational waves emitted by unstable neutron star oscillations can be used to obtain information about their inner structure, that is, the equation of state of dense nuclear matter. After its initial growth phase, the instability is expected to saturate due to nonlinear effects. The saturation amplitude of the unstable mode determines the detectability of the generated gravitational-wave signal, but also affects the evolution of the neutron star. The study shows that the unstable (parent) mode resonantly couples to pairs of stable (daughter) modes, which drain the parent's energy and make it saturate via a mechanism called parametric resonance instability. Further, it calculates the saturation amplitude of the most unstable f-mode multipoles throughout their so-called instability windows.
000856302 588__ $$aOnline resource; title from PDF title page (SpringerLink, viewed October 3, 2018).
000856302 650_0 $$aNeutron stars.
000856302 77608 $$iPrint version:$$aPnigouras, Pantelis.$$tSaturation of the f-mode instability in neutron stars.$$dCham, Switzerland : Springer, 2018$$z3319982575$$z9783319982571$$w(OCoLC)1044838603
000856302 830_0 $$aSpringer theses.
000856302 852__ $$bebk
000856302 85640 $$3SpringerLink$$uhttps://univsouthin.idm.oclc.org/login?url=http://link.springer.com/10.1007/978-3-319-98258-8$$zOnline Access$$91397441.1
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