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	Quasinormal mode: Encyclopedia with 57,959 entries from biotech, medicine & life sciences.
		Quasinormal modes (QNM) are the modes of energy dissipation of a perturbed object or field.
		In theoretical physics, a quasinormal mode is a formal solution of linearized differential equations (such as the linearized equations of general relativity constraining perturbations around a fl hole solution) with a complex eigenvalue (frequency).
		quasinormal modes in the context of the AdS/CFT correspondence
	www.bionity.com /lexikon/e/Quasinormal_mode (331 words)

	Quasinormal mode - Wikipedia, the free encyclopedia
		Quasinormal modes (QNM) are the modes of energy dissipation of a perturbed object or field.
		In theoretical physics, a quasinormal mode is a formal solution of linearized differential equations (such as the linearized equations of general relativity constraining perturbations around a fl hole solution) with a complex eigenvalue (frequency).
		quasinormal modes in the context of the AdS/CFT correspondence
	en.wikipedia.org /wiki/Quasinormal_mode (325 words)

	The Reference Frame: Quasinormal story on quasinormal modes
		In this case, there are "metastable" modes in which the particle sits in the "hole" for quite a long time, but eventually it escapes by quantum tunneling (the rate of the tunneling exponentially depends on the parameters, which is why the lifetime of various alpha-decays are so incredibly diverse in size).
		The role of quasinormal modes in the context of string theory and especially the AdS/CFT correspondence was studied in many serious papers, starting from pioneering works such as the article of Horowitz and Hubeny.
		The first working method to prove that "ln(3)" appears in the quasinormal modes was based on the analysis of the behavior of the continued fractions and their critical behavior - plus patching different partial solutions together.
	motls.blogspot.com /2005/03/quasinormal-story-on-quasinormal-modes.html (4289 words)

	[No title]
		Zerilli and Psi4 waveforms and modefit with the 12 quasinormal modes determined by Yoshida, Eriguchi and Futamase, 1994
		This is due to the results of [Yoshida, Eriguchi and Futamase, 1994] in which quasinormal modes frequencies with both real and imaginary parts are found to exist for various models of boson stars.
		Quasinormal Modes of l=2 for a Stable Boson Star of central density 0.1414 [Yoshida, Eriguchi and Futamase, 1994]
	astrosun2.astro.cornell.edu /~ruxandra/Data_Dec1/boson.html (575 words)

	Quasinormal modes (Site not responding. Last check: 2007-10-23)
		Quasinormal modes are the natural frequencies of a perturbed object or a field.
		One might be tempted to call those modes normal but no. The glass does not go on ringing forever, amplitude of oscillation decays in time; we therefore call the modes of sonic radiation it emanates quasi-normal.
		Where omega is what is commonly referred to as the quasinormal mode.
	www.physics.unc.edu /~hbar/work/qnm (202 words)

	[No title] (Site not responding. Last check: 2007-10-23)
		Of particular interest is a set of complex frequencies, the quasinormal modes, that describe in part the temporal behaviour of perturbations.
		Quasinormal modes are interesting because they are characteristic only of the fl hole and are not sensitive to the initial conditions of the perturbation.
		They are in some sense analogous to modes of leaky optical cavities or of musical instruments.
	www.iqis.org /seminars/abstract.php?id=82 (145 words)

	Luboš Motl's reference frame: Quasinormal story on quasinormal modes (Site not responding. Last check: 2007-10-23)
		In this case, there are "metastable" modes in which the particle sits in the "hole" for quite a long time, but eventually it escapes by quantum tunneling (the rate of the tunneling exponentially depends on the parameters, which is why the lifetime of various alpha-decays are so incredibly diverse in size).
		The role of quasinormal modes in the context of string theory and especially the AdS/CFT correspondence was studied in many serious papers, starting from pioneering works such as the article of Horowitz and Hubeny.
		The first working method to prove that "ln(3)" appears in the quasinormal modes was based on the analysis of the behavior of the continued fractions and their critical behavior - plus patching different partial solutions together.
	schwinger.harvard.edu /~motl/blog/2005/03/quasinormal-story-on-quasinormal-modes.html (4215 words)

	Physics at Minnesota: Physics and Astronomy Calendar
		It has been suggested that there may exist a connection between the highly damped quasinormal modes of fl holes and the semi-classical level spacing in the fl hole quantum area spectrum.
		It is therefore crucial to understand the physical/mathematical nature of the highly damped quasinormal modes in as many different situations as possible.
		We calculate analytically the highly damped quasinormal mode spectra of generic single-horizon fl holes using the rigorous WKB techniques of Andersson and Howls.
	www.physics.umn.edu /calendar/all/calendar.html?item=1874 (221 words)

	WUGRAV -- Washington University Gravity Group
		Nonlinear r-Modes in Neutron Stars: Instability of an unstable mode
		Quasi-Normal Modes of General Relativistic Superfluid Neutron Stars
		Wave Propagation in Gravitational Systems: Completeness of Quasinormal Modes
	wugrav.wustl.edu /research/papers/index.php?showall=1&showdetail=0 (341 words)

	Department of Physics at the University of Florida :: FACULTY LISTING (Site not responding. Last check: 2007-10-23)
		While commencing in the domain of classical general relativity, this work now includes semi-classical results pertaining to a quantum theory of gravity, has concerned both perturbative and non-perturbative effects in fl hole thermodynamics, and involves ongoing work on the final state of fl hole evaporation.
		A key result in classical general relativity was the proof of the mode stability of the Kerr fl hole (J.
		This work has also required the study of quantum mechanics for very simple interest in describing the early universe adequately enough to be able to evaluate its impact on our observations of the cosmos as we no find it.
	www.phys.ufl.edu /faculty/whiting.html (298 words)

	vallis.org: Michele's wikiblog
		The detectability of different modes depends on their relative excitation, which in turn depends on the cause of the perturbation (i.e.
		A ‘universal’, initial data-independent measure of the relative mode excitation is encoded in the poles of the Green's function that propagates small perturbations of the geometry (‘excitation factors’).
		We find that for corotating modes with $l=m$ the excitation factors tend to zero in the extremal limit, and that the contribution of the overtones should be more significant when the fl hole is fast rotating.
	www.vallis.org /blogspace/preprints/2006/05 (2302 words)

	CFC
		Quasinormal modes and classical wave propagation in analogue fl holes
		We compute the quasinormal mode frequencies of this system and discuss late-time power-law tails.
		Finally we discuss quasinormal modes and late-time tails in a non-rotating canonical acoustic fl hole, corresponding to an incompressible, spherically symmetric (3+1)-dimensional fluid flow.
	cfc.fis.uc.pt /public.php?oid=3975656 (131 words)

	Roberto Gómez / Current Research Page
		The amplitudes of the scalar and gravitational outgoing radiation modes exhibit the predicted power law scaling with respect to the amplitude of the initial data.
		For the scattering of an axisymmetric scalar field, the final ring down matches the complex frequency calculated perturbatively for the $\ell=2$ quasinormal mode.
		Feature (ii) is unexpected and has the potential importance of enabling the design of an efficient template for extracting the gravitational wave signal from the noise.
	www.psc.edu /~gomez/research.html (2182 words)

	Methods for 3-D vector microcavity problems involving a planar dielectric mirror (ResearchIndex) (Site not responding. Last check: 2007-10-23)
		2 Mode structure and ray dynamics of a parabolic dome microcav..
		2 Astigmatic laser mode converters and transfer of orbital ang..
		Mode Structure and Ray Dynamics of a Parabolic Dome Microcavity - Nöckel (2002)
	citeseer.ist.psu.edu /foster04methods.html (391 words)

	APS - 2005 APS April Meeting - Event - Evolution of 3D Boson Stars with Waveform Extraction (Site not responding. Last check: 2007-10-23)
		We study the evolution of stable, critical and unstable boson stars subjected to various types of nonspherical perturbations and analyze the emitted gravitational waves.
		We calculate the Zerilli and Newman-Penrose $\Psi_4$ gravitational waveforms and study the quasinormal mode content of the numerical waveforms using predicted QNM frequencies from perturbation theory calculations of Yoshida, Eriguchi and Futamase.
		The apparent horizons formed from perturbed unstable star collapse were observed to be slightly nonspherical when initially detected and became more spherical as the system evolved.
	meetings.aps.org /Meeting/APR05/Event/29292 (181 words)

	reserach_Bekenstein.html (Site not responding. Last check: 2007-10-23)
		In the last decade various workers have noticed an interesting systematics in the (classical) quasinormal mode frequencies of various types of fl holes, the ''ringing frequencies'' of a fl hole.
		Hod combined this suggestion with our connection with the fl hole entropy and noticed that the quasinormal frequencies of the Schwarzschild fl hole correspond exactly to what was expected if the logarithm is ln(3).
		This has led to a lot of analytic work on the quasinormal modes, as well as to a bounty of numerical results.
	www.fiz.huji.ac.il /~bekenste/research_Bekenstein.html (1746 words)

	[No title]
		Nollert's original calculation appears in 11) Hans-Peter Nollert, Quasinormal modes of Schwarzschild fl holes: the determination of quasinormal frequencies with very large imaginary parts, Phys.
		Technically the vibrational modes of a fl hole are called "quasinormal modes".
		In loop quantum gravity, the area eigenvalues get very densely packed for a large fl hole, since one is adding up lots of different numbers of the form 8 pi gamma sqrt(j(j+1)), so one would not see widely spaced spectral lines in Hawking radiation from a large fl hole.
	math.ucr.edu /home/baez/twf_ascii/week189 (4093 words)

	IngentaConnect Highly damped quasinormal modes of generic single-horizon black h... (Site not responding. Last check: 2007-10-23)
		IngentaConnect Highly damped quasinormal modes of generic single-horizon fl h...
		Highly damped quasinormal modes of generic single-horizon fl holes
		We calculate analytically the highly damped quasinormal mode spectra of generic single-horizon fl holes using the rigorous WKB techniques of Andersson and Howls (2004 Class.
	www.ingentaconnect.com /content/iop/cqg/2005/00000022/00000019/art00020 (175 words)

	mordor
		If the ligand binds preferentially to the induced-fit state with sufficiently favorable free energy change, i.e., greater than the free energy difference between the native and induced-fit states of the macromolecule, the average structure of the macromolecule will change.
		If the ligand is capable of multiple binding modes to a macromolecule (binding to different folded forms or multiple binding sites of a single form), it may be necessary to account for these additional states to predict affinity properly.
		An entropy term which will be derived from a quasinormal mode calculation.
	mondale.ucsf.edu /science/mordor.html (1371 words)

	Re: Black holes and Barbero-Immirzi
		modes to fl hole entropy is not the SU(2) versus SO(3) business.
		be related to quasinormal modes as in the nonrotating case.
		to thermal modes, i.e., with characteristic periodicities in imaginary
	www.physicsforums.com /showthread.php?p=218213 (769 words)

	vallis.org: Michele's wikiblog
		From the ring-down portion of the GW we extract the fundamental quasi-normal mode and several of the overtones.
		{\bf 631}, 495 (2005)], we are able to determine the mass, the radius and the mass distribution of a star from its quasi-normal mode frequencies of stellar pulsation.
		In addition, accurate equation of state of nuclear matter can be obtained from such inversion scheme.
	www.vallis.org /blogspace/preprints/gr-qc (3199 words)

	The Cactus Code - Numerical Relativity Publications
		A numerical study of the quasinormal mode excitation of kerr fl holes.
		Mode coupling in the nonlinear response of fl holes.
		Nonlinear and perturbative evolution of distorted fl holes: Odd-parity modes.
	www.cactuscode.org /Papers/NumRel (1877 words)

	AdS/Au-Au II \| Musings
		This, apparently, is the upper limit on the viscous damping parameter, and may be universal.
		But it’s a little unclear that one should trust the quasinormal mode analysis in this limit, as quantum fluctuations of the short string are important, in contrast to the long-string (heavy-quark) limit.
		The calculation involved is similar to our quasinormal mode calculation, but the interpretation involves the Schwinger-Keldysh formalism.
	golem.ph.utexas.edu /~distler/blog/archives/000820.html (942 words)

	Quasinormal modes for single horizon black holes in generic 2D dilaton gravity
		Quasinormal modes for single horizon fl holes in generic 2D dilaton gravity
		There has been some recent speculation that a connection may exist between the quasinormal-mode spectra of highly damped fl holes and the fundamental theory of quantum gravity.
		However, even if the level spacing can be fixed in this manner, it still remains unclear whether this implies a physically significant 'duality' or merely a numerical coincidence.
	stacks.iop.org /0264-9381/21/5317 (340 words)

	Cardiff Relativity Group Papers (Site not responding. Last check: 2007-10-23)
		Quasinormal modes and the grin of the Cheshire cat
		Quasinormal modes of Reissner-Nordstrom fl holes: Phase-integral approach
		A new numerical approach to the oscillation modes of relativistic stars
	www.astro.cf.ac.uk /groups/relativity/papers/papers.html (273 words)

	AstroGravS: Literature Catalog: Black Hole Ringdown Sources
		Kokkotas and B. Schmidt, Quasi-normal modes of stars and fl holes, Living Rev. Rel.
		Onozawa, A detailed study of quasinormal frequencies of the Kerr fl hole, Phys.
		Andersson and H. Onozawa, Quasinormal modes of nearly extreme Reissner-Nordstroem fl holes, Phys.
	astrogravs.gsfc.nasa.gov /docs/lit/ringdown_date.html (1114 words)

	Publications: Can you hear the shape of a bell?: asymptotics of quasinormal modes
		Can you hear the shape of a bell?: asymptotics of quasinormal modes
		The spectrum of gravitational waves emitted after the formation of a fl hole is dominated by damped oscillations, or ringing tones, represented by quasinormal modes.
		An analogy with the natural frequencies of a bell is quite fitting, since any system with a continuous spectrum permits complex frequency resonances.
	www.phys.ncl.ac.uk /research/pubs/abs155.htm (129 words)

	The asymptotic quasinormal mode spectrum of non-rotating black holes
		The asymptotic quasinormal mode spectrum of non-rotating fl holes
		A conjectured connection to quantum gravity has led to a renewed interest in highly damped fl-hole quasinormal modes (QNMs).
		In this paper we present simple derivations (based on the WKB approximation) of conditions that determine the asymptotic QNMs for both Schwarzschild and Reissner–Nordström fl holes.
	stacks.iop.org /0264-9381/21/1623 (283 words)

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