Gauge invariance of general relativistic tidal heating

Purdue, Patricia

doi:10.1103/physrevd.60.104054

Cited by 25 publications

(70 citation statements)

References 17 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…(10.8) and (10.9). Assuming the form of the metric used in the pseudotensorial calculations, for the tidal work they recovered the gauge invariant expressions obtained in [432, 185]. In these approximate calculations the precise form of the boundary conditions (or reference configurations) is not essential, because the results obtained by using different boundary conditions deviate from each other only in higher order.…”

Section: Applications In General Relativitymentioning

confidence: 74%

“…However, gravitational energy (both in Newtonian theory and in general relativity) is only ambiguously defined (and hence, cannot be localized), while the phenomena mentioned above cannot depend on the mathematics that we use to describe them. The first investigations intended to calculate the tidal work (or heating) of a compact massive body were based on the use of various gravitational pseudotensors [432, 185]. It has been shown that, although in the given (slow motion and isolated body) approximation the interaction energy between the body and its companion is ambiguous, the tidal work that the companion does on the body via the tidal forces is not.…”

Section: Applications In General Relativitymentioning

confidence: 99%

“…It has been shown that, although in the given (slow motion and isolated body) approximation the interaction energy between the body and its companion is ambiguous, the tidal work that the companion does on the body via the tidal forces is not. This is independent of both the gauge conditions [432] and the actual pseudotensor (Einstein, Møller, Bergmann, or Landau-Lifshitz) [185]. …”

Section: Applications In General Relativitymentioning

confidence: 99%

See 2 more Smart Citations

Quasi-Local Energy-Momentum and Angular Momentum in General Relativity

Szabados

2009

Living Rev. Relativ.

330

390

View full text Add to dashboard Cite

The present status of the quasi-local mass, energy-momentum and angular-momentum constructions in general relativity is reviewed. First, the general ideas, concepts, and strategies, as well as the necessary tools to construct and analyze the quasi-local quantities, are recalled. Then, the various specific constructions and their properties (both successes and deficiencies are discussed. Finally, some of the (actual and potential) applications of the quasi-local concepts and specific constructions are briefly mentioned.

show abstract

Section: Applications In General Relativitymentioning

confidence: 74%

Section: Applications In General Relativitymentioning

confidence: 99%

Section: Applications In General Relativitymentioning

confidence: 99%

See 1 more Smart Citation

Quasi-Local Energy-Momentum and Angular Momentum in General Relativity

Szabados

2009

Living Rev. Relativ.

330

390

View full text Add to dashboard Cite

show abstract

“…However, gravitational energy (both in Newtonian theory and in general relativity) is only ambiguously defined (and hence cannot be localized), while the phenomena mentioned above cannot depend on the mathematics that we use to describe them. The first investigations intended to calculate the tidal work (or heating) of a compact massive body were based on the use of the various gravitational pseudotensors [318, 136]. It has been shown that although in the given (slow motion and isolated body) approximation the interaction energy between the body and its companion is ambiguous, the tidal work that the companion does on the body via the tidal forces is not.…”

Section: Applications In General Relativitymentioning

confidence: 99%

Quasi-Local Energy-Momentum and Angular Momentum in GR: A Review Article

Szabados

2004

Living Rev. Relativ.

321

528

View full text Add to dashboard Cite

The present status of the quasi-local mass-energy-momentum and angular momentum constructions in general relativity is reviewed. First the general ideas, concepts, and strategies, as well as the necessary tools to construct and analyze the quasi-local quantities are recalled. Then the various specific constructions and their properties (both successes and defects) are discussed. Finally, some of the (actual and potential) applications of the quasi-local concepts and specific constructions are briefly mentioned.This review is based on the talks given at the Erwin Schrödinger Institute, Vienna, in July 1997, at the Universität Tübingen, in May 1998, and at the National Center for Theoretical Sciences in Hsinchu and at the National Central University, Chungli, Taiwan, in July 2000.

show abstract

“…V. The energy conservation method is simpler to use than the method of integration of the See Refs. [65][66][67][68] for further discussion of the derivation method and of similar tidal work formulas.…”

Section: Effect Of Current Quadrupole On Orbital Motionmentioning

confidence: 99%

Gravitomagnetic resonant excitation of Rossby modes in coalescing neutron star binaries

2007

View full text Add to dashboard Cite

In coalescing neutron star binaries, r-modes in one of the stars can be resonantly excited by the gravitomagnetic tidal field of its companion. This post-Newtonian gravitomagnetic driving of these modes dominates over the Newtonian tidal driving previously computed by Ho and Lai. To leading order in the tidal expansion parameter R=r (where R is the radius of the neutron star and r is the orbital separation), only the l 2, jmj 1, and jmj 2 r-modes are excited. The tidal work done on the star through this driving has an effect on the evolution of the inspiral and on the phasing of the emitted gravitational wave signal. For a neutron star of mass M, radius R, spin frequency f spin , modeled as a ÿ 2 polytrope, with a companion also of mass M, the gravitational wave phase shift for the m 2 mode is 0:1 radians R=10 km 4 M=1:4M ÿ10=3 f spin =100 Hz 2=3 for optimal spin orientation. For canonical neutron star parameters this phase shift will likely not be detectable by gravitational wave detectors such as LIGO, but if the neutron star radius is larger it may be detectable if the signal-to-noise ratio is moderately large. The energy transfer is large enough to drive the mode into the nonlinear regime if f spin * 100 Hz. For neutron star-black hole binaries, the effect is smaller; the phase shift scales as companion mass to the ÿ4=3 power for large companion masses. The net energy transfer from the orbit into the star is negative corresponding to a slowing down of the inspiral. This occurs because the interaction reduces the spin of the star, and occurs only for modes which satisfy the ChandrasekharFriedman-Schutz instability criterion. A large portion of the paper is devoted to developing a general formalism to treat mode driving in rotating stars to post-Newtonian order, which may be useful for other applications. We also correct some conceptual errors in the literature on the use of energy conservation to deduce the effect of the mode driving on the gravitational wave signal.

show abstract

Gauge invariance of general relativistic tidal heating

Cited by 25 publications

References 17 publications

Quasi-Local Energy-Momentum and Angular Momentum in General Relativity

Quasi-Local Energy-Momentum and Angular Momentum in General Relativity

Quasi-Local Energy-Momentum and Angular Momentum in GR: A Review Article

Gravitomagnetic resonant excitation of Rossby modes in coalescing neutron star binaries

Contact Info

Product

Resources

About