Propagation
of Gravitational Radiation| Propagation
of Gravitational Radiation |
In General > s.a. dark
matter; decoherence; lensing; relativistic
cosmology.
* Idea: Gravitational
waves are not absorbed or scattered almost at all, which is bad news for
their detection but good for the possibility of using them to observe phenomena
that would otherwise be hidden.
* Christodoulou effect:
A true non-linearity due to the fact that a gravitational wave produces itself
new gravitational waves.
@ General references: Arnowitt et al PR(61)
[wave zone]; Thorne gq/97-in.
@ Speed: McDonald AJP(97);
Baskaran et al a0805 [from pulsar timing].
@ Dispersion: in Szekeres AP(71); Prasanna PLA(99) [dispersive medium].
@ (Almost) spherical wavefronts: Sharif NCB(01)gq [momentum];
Hayward CQG(01)gq.
@ And cmb: Seljak & Zaldarriaga PRL(97)ap/96 [polarization];
Durrer & Kahniashvili
HPA(98)ap/97.
@ Other effects: Fakir ap/96,
IJMPD(97)
[pulsar signals]; Faraoni IJMPD(98)ap/97, & Gunzig
A&A(98)ap [as
gravitational lenses]; Novello et al PLA(99)
[with speed v < c]; Macquart ap/06/A&A
[scattering by stars
and inhomogeneities]; Congedo et al IJMPD(06),
Longo et al ap/06-in
[diffraction by cluster]; Kocsis & Loeb PRD(07)-a0704
[contraction
from self-gravity]; Liu a0706 [no
energy dissipation in vacuum from quantum field theory]; > s.a. Sagnac
Effect.
Specific Types of Spacetimes > s.a. topological
defects.
@ In FRW: Bicák & Griffiths AP(96)gq;
Dunsby et al CQG(97);
Hogan & O'Shea PRD(02)gq,
O'Shea PRD(04), PRD(04);
Balek & Polák a0707 [superluminal group velocity].
@ Other backgrounds: Hogan & O'Shea PRD(02)gq [in
Bianchi I]; Easther et al
JCAP(03)ht [Randall-Sundrum
cosmology].
Effects on Matter
@ Particles: Kleidis CQG(96)gq/99 [particle
resonant acceleration]; Papadopoulos GRG(04)gq/03 [spinning
charged particle in B]; Voyatzis et al PLA(06)
[acceleration].
@ Other effects: Ingraham GRG(97)
[general propagation]; Asada & Futamase
PRD(97)gq;
Sharif ASS(97)gq/07 [imparted
angular momentum]; Chicone et al JPA(00)
[binary system]; Malec & Schäfer
PRD(01)gq [black
hole]; Licht gq/04 [conductors];
Tammelo & Mullari GRG(06)
[pressure].
And Electromagnetic Fields / Waves > s.a. polarization.
* In magnetized plasmas:
The interaction can lead to damping of the gravitational wave and growth of
plasma waves.
@ Magnetic fields:
Maartens et al PRD(01)ap;
Moortgat & Kuijpers gq/04-in,
gq/05-in,
Isliker et al PRD(06)ap [magnetized
plasma].
@ Related topics: Marklund et al PRD(00)gq [waves];
Balakin et al CQG(01)gq/00 [Cerenkov
radiation]; Chiao & Fitelson gq/03-in
[and electromagnetic waves]; Alekseev & Griffiths CQG(04)gq
[collisions between waves].
Gravitational Wave Tails
* Idea: Produced by scattering in the propagation in a curved background.
* Calculation: One can
use the Direct Integration of the Relaxed Einstein Equations (DIRE).
@ References: Christodoulou PRL(91);
Wiseman & Will PRD(91); Blanchet & Schäfer CQG(93);
Blanchet & Sathyaprakash
CQG(94),
PRL(95);
Blanchet
CQG(98)gq/97 [tails
of tails]; Khriplovich & Pomeransky PLA(99)gq/97;
Epstein & Wagoner, Will PTPS(99)gq-in
[DIRE].
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Send feedback and suggestions to bombelli at olemiss.edu – Modified
21 jun 2008