Gravitational Waves: Volume 1: Theory and Experiments

By M. Maggiore. 2007

506 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/4f5a454341a52f88697c0a59457e39760c600b9c

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In Astronomy and Astrophysics

Citations in the corpus

Open data from the first and second observing runs of Advanced LIGO and Advanced Virgo (2019, unknown): “variations of the mass quadrupole [1], as in the orbital motion of a binary system of compact stars.”
The stochastic gravitational wave background from turbulence and magnetic fields generated by a first-order phase transition (2009, background): “ion with =H = 100, T = 100 GeV, v f = 1= p 3 and v b’0:87. The peak amplitude for the above values of the parameters is h2 0 peak GW(K ) ’10 11. Using that h(f) = 1:26 10 15 p h2 0 GW(f)(mHz=f) (see [63]), we obtain the maximal GW amplitude h(f peak) ’2 10 21 which is detectable with LISA (see Fig. ”
Induced gravitational waves in a general cosmological background (2019, background): “The large line on top of the expectation value refers to oscillation average(4) and estimates the observed amplitude of the stochastic background [35, 85].”
Beyond the Standard Models with cosmic strings (2019, background): “ency is determined from NG simulations, ’50 [106]. Note that the gravitational power radiated by a loop is independent of its length. This can be understood from the quadrupole formula P = G=5(Q000)2 [28,107] where the triple time derivative of the quadrupole, Q000/mass(length)2=(time)3 /, is indeed”
A Massive Pulsar in a Compact Relativistic Binary (2013, background): “04 (NS-BH) cycles, an amount that would not jeopardize the detection of the gravitational wave signal in the LIGO/VIRGO band (37).”
Challenges and opportunities of gravitational-wave searches at MHz to GHz frequencies (2020, methodology): “Depending on the source/detector, the strength of GWs, detector noise, and signalto-noise ratio are described using various different metrics (Maggiore 2007).”
ZAIGA: Zhaoshan long-baseline atom interferometer gravitation antenna (2019, methodology): “To illuminate the response of a detector to a GW signal, we choose a binary system in spiral time domain waveform as follows [49]”
Expected properties of the first gravitational wave signal detected with pulsar timing arrays (2015, unknown): “According to General Relativity, accelerating masses with a mass quadrupole moment varying in time generate GWs, and our Universe has plenty of systems fulfilling such a requirement (Wald 1983; Maggiore 2008); from compact binaries (emitting GWs while inspiraling towards one another until coalescenc”
Towards a generic test of the strong field dynamics of general relativity using compact binary coalescence: Further investigations (2011, background): “, the discussion in [19] and references therein.”