Detection
of Gravitational Waves| Detection
of Gravitational Waves |
In General > s.a. [gravitational
radiation]; graviton; sources.
* Motivation: Their
detection will give, in addition to new tools for astronomy and possible
unexpected effects, (i) Direct evidence for time-varying metrics; (ii) Spin
and polarization, rest mass and velocity of gravitons; (ii) Tests of strong-field
general relativity
and black holes – wave
forms and df/dt will probe black-hole geometry and test
no-hair theorems, general relativity makes precise predictions re overtones
in
ringing; (iv) Inner dynamics of stars hidden from electromagnetic observations;
(v) Insight into Planck era physics.
* Idea: Although
gravitational waves produce very small effects, our detection methods measure
their amplitude rather than their intensity, and their amplitude decreases
more slowly with distance from the source.
* Status: 1989, Binary
pulsar data and general relativity agree to 1% (2+1/2 order in PN); Prediction
that it will be possible to detect radiation from collapse in the Virgo
Cluster
in this century [turned out to be wrong]; 2004, New Scientist sets the chances of
detection
by 2010 at 500/1, 5 times less likely than finding Elvis alive.
Resonant Bar Antennas
* Original Weber bar:
A large freely suspended bar oscillating longitudinally on resonance (use SQUIDs,
with motion detected by a transducer); 1986 sensitivities
(
L)/L of
about 10–18 (enough
only for rare events in our galaxy); Sufficient (40 mK) cooling of the bar
and low-noise
SQUIDs could give about 3 
10–21,
from zero-point motion.
* Spherical bar detectors: Truncated icosahedra; Motivated by their
directional resolution.
* 2000: The IGEC (International
Gravitational Event Collaboration), the first ever network of 5-m, 2000-kg
cryogenic resonant-cylinder gravity wave detectors, is now operational;
It consists of five widely spaced detectors, one in the US (ALLEGRO,
in Baton Rouge), two
in Italy (Auriga and NAUTILUS, in Legnaro and Frascati),
one at CERN (Explorer), and one in Australia (Niobe, in Perth);
It is setting bounds on events in our galaxy.
* 2006: Plans for spherical
detectors, e.g., MiniGRAIL.
@ General references: Mauceli et al PRD(96)
[ALLEGRO]; Astone et al PRL(00), PLB(01)
[NAUTILUS, cosmic rays]; Frasca gq/00-in
[status]; Allen et al PRL(00)
[bursts]; Finn CQG(03)gq [comments
on status]; Sisto & Moleti IJMPD(04)
[sensitivity]; Astone et al PRD(07)
[IGEC-2 search for bursts]; AURIGA & Virgo CQG(08)-a0801 [cross-correlation
method].
@ Spherical: Briant et al PRD(03)gq [nested
spheres]; Gasparini PRD(05)gq [performance];
Magalhaes et al PRD(05)
[lightning]; Costa & de Aguiar gq/06/PRD
[analysis].
@ Acoustic detectors: Lobo PRD(95)gq/00;
Finn gq/96-in;
Lobo & Montero
CQG(02)gq [stochastic
background].
Other Methods > s.a. interferometers and
space-based detectors.
* MIGO: Matter-wave interferometers, using atomic beams emanating
from supersonic atomic sources that are further cooled and collimated by means
of
optical molasses; The sensitivities compare favorably with LIGO
and LISA, but the sizes of MIGOs can be orders of magnitude smaller,
and
their bandwidths wider.
* Indirect methods: One
includes monitoring binary pulsars over long periods of time and finding small
residual variations in the signal that can be attributed to fluctuations in
the metric near the system.
@ Using light: Bergmann PRL(71);
Mitskiewich & Nesterov GRG(95)
[geometric phase]; Tamburini et al a0804 [photon entangled states].
@ Superconductors: Gemme et al gq/01-in
[coupled cavities]; Chiao gq/02-in
[Meißner-like effect], gq/02-in;
Golovashkin gq/03-in;
Chiao et al a0903.
@ Using storage rings: Zer-Zion APP(00); Ivanov & Kobushkin
gq/02.
@ MIGO: Chiao & Speliotopoulos JMO-gq/03;
Roura et al PRD(06)gq/04 [no
better than LIGO]; Dimopoulos et al PLB(09)-a0712,
PRD(08)-a0806.
@ Related topics: Fakir ap/95 [precision
astrometry]; Karim gq/02 [compact
detector??]; Brodin & Marklund CQG(03)
[cavity electromagnetic waves]; Lesovik et
al PRD(05)ap [light
phase modulation]; Chiao JMO-qp/06-in
[charged superfluids], IJMPD(08)gq/06-in
+ gq/06-in,
gq/07, a0904 ["Millikan
oil drops"]; Armstrong LRR(06)
[spacecraft Doppler tracking]; Daishev et al gq/06 [Dulkyn
project]; > s.a. torsion.
Applications and Other Effects > s.a. gravitational-wave
propagation; wave phenomena.
@ Neutron stars: Faber et al PRL(02)ap [equation
of state and size].
@ Cosmology: Schutz gq/01-in; > s.a. cosmological
acceleration; observational
cosmology.
@ Early-universe cosmology: Maggiore PRP(00).
@ GRBs: Finn et al PRD(99)gq [GRBs];
news pw(08)jan
[no detection by LIGO].
@ Response of bodies: Carter in(83)gq/01 [elastic
solid]; Hannibal & Warkall
gq/00 [massive
bodies]; Baskaran & Grishchuk CQG(04)gq/03.
References > s.a. radiation and
interferometers [analysis]; {Talk by K Thorne at SU, 1985}.
@ Elementary: Davies; Shapiro et al AS(85);
Abrahams & Shapiro
ThSc(90)jul; NS(90)sep1,
p30-34; Ruthen SA(92)mar;
Schäfer & Schutz
PW(96); Bartusiak 00; Caldwell & Kamionkowski SA(01)jan;
Gibbs SA(02)apr; Shawhan AS(04).
@ Reviews: Braginsky & Rudenko PRP(78);
Douglass & Braginsky
in(79); Thorne RMP(80);
Tinto AJP(88)dec;
Grishchuk SPU(88); Schutz CQG(89);
Blair ed-91;
Thorne gq/95,
in Texas XVII(95), gq/97;
Ju & Blair IJMPD(96);
Flanagan gq/98-GR15;
Ricci CP(98);
Finn et al gq/99;
Grishchuk et al SPU(01)ap/00;
Sathyaprakash Pra(01)gq/00-in;
Finn gq/01;
Harry et al PRD(02)gq/01 [comparison];
Lobo LNP-gq/02;
Bezrukov et al gq/04-in;
Hough et al JPB-gq/05;
Aufmuth & Danzmann NJP(05);
Hogan a0709-in
[future]; Kokkotas a0809;
Fairhurst et al a0908-GRG.
@ Conceptual discussion re possibility of detection: Saulson AJP(97)jun
[II]; Garfinkle AJP(06)mar-gq/05; Leclerc gq/06;
Faraoni GRG(07)gq; Corda a0706.
@ Analysis: Finn gq/97-in
[statistical inference]; 10th Workshop CQG(06)#19;
Robinson et al PRD(08)-a0804 [network
data and coincidences]; Littenberg & Cornish PRD(09)-a0902 [Bayesian
approach]; Jaranowski & Krolak 09; Yunes & Pretorius a0909/PRD
[theoretical bias and post-Einsteinian framework]; GWDAW13 CQG(09)#20.
@ With scalar waves: Maggiore & Nicolis PRD(00)gq/99;
Fucito gq/00-in;
Bellucci et al PLA(01)ht;
Babusci et al PRD(01)gq [stochastic
background]; Capozziello & Corda IJMPD(06)
[scalar-tensor, production and detection]; Corda gq/06 [interferometer response].
@ And electromagnetic / photon astronomy: Bloom et al a0902-rp
[Astro2010]; Owen CQG(09)-a0904-in.
@ Related topics: Anandan PLA(85)
[using superconducting circuits]; Fortini et al AP(96)gq/98 [electric
circuits]; Maggiore gq/98 [hep];
Rizzi GRG(02)
[spacetime stretching]; Fargion
ap/04-in
[tsunamis];
Collins 04 [history, sociology]; Braginsky et al PLA(06)
[cosmic ray noise]; Van Elewyck et al a0906-in
[joint search with neutrino telescopes]; Searle et al CQG(09) [detection of unmodeled
sources].
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send feedback and suggestions to bombelli at olemiss.edu – modified 10
oct 2009