Mixing and reaction efficiency in closed domains

Berti, Stefano; Vergni, Davide; Visconti, Francesco; Vulpiani, Angelo

doi:10.1103/physreve.72.036302

Cited by 17 publications

(48 citation statements)

References 26 publications

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“…For LISA, the GW bound could improve significantly, due to the lower frequencies and higher distances, possibly reaching m g < 10 −26 eV/c 2 [339]. In addition, there are proposals to bound m g measuring the phase lag of continuos sources of GWs and EM radiation with LISA binaries [340][341][342].…”

Section: B Mass Termmentioning

confidence: 99%

Dark Energy in Light of Multi-Messenger Gravitational-Wave Astronomy

Ezquiaga

Zumalacárregui

2018

Front. Astron. Space Sci.

209

202

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Gravitational waves (GWs) provide a new tool to probe the nature of dark energy (DE) and the fundamental properties of gravity. We review the different ways in which GWs can be used to test gravity and models for late-time cosmic acceleration. Lagrangian-based gravitational theories beyond general relativity (GR) are classified into those breaking fundamental assumptions, containing additional fields and massive graviton(s). In addition to Lagrangian based theories we present the effective theory of DE and the µ-Σ parametrization as general descriptions of cosmological gravity. Multi-messenger GW detections can be used to measure the cosmological expansion (standard sirens), providing an independent test of the DE equation of state and measuring the Hubble parameter. Several key tests of gravity involve the cosmological propagation of GWs, including anomalous GW speed, massive graviton excitations, Lorentz violating dispersion relation, modified GW luminosity distance and additional polarizations, which may also induce GW oscillations. We summarize present constraints and their impact on DE models, including those arising from the binary neutron star merger GW170817. Upgrades of LIGO-Virgo detectors to design sensitivity and the next generation facilities such as LISA or Einstein Telescope will significantly improve these constraints in the next two decades.

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Section: B Mass Termmentioning

confidence: 99%

Dark Energy in Light of Multi-Messenger Gravitational-Wave Astronomy

Ezquiaga

Zumalacárregui

2018

Front. Astron. Space Sci.

209

202

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“…On the other edge of the frequency spectrum, f min is limited by seismic noise for ground based detectors, f LIGO/Virgo min = 10 Hz, f ET min = 3 Hz, while we fix f min = 0.01 Hz for B-DECIGO [27]. Finally, following [77] the initial frequency for LISA is determined by:…”

Section: A Signal-to-noise Ratios and The Fisher Matrixmentioning

confidence: 99%

Bounding alternative theories of gravity with multiband GW observations

et al. 2019

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We study the constraints on alternative theories of gravity that can be determined by multi-band observations of gravitational wave signals emitted from binary black hole coalescences. We focus on three types of General Relativity modifications induced by a generalised Brans-Dicke theory, and two classes of quadratic gravity, Einstein-dilaton-Gauss-Bonnet and dynamical Chern-Simons. Considering a network of space and ground-based detectors, supplied by a population of spinning binaries black hole, we show how the multi-band analysis improves the existing bounds on the theory's parameters by several orders of magnitude, for both pre-and post-Newtonian deviations. Our results also show the fundamental role played by an interferometer in the frequency range between LISA and advanced detectors, in constraining possible deviations from General Relativity.

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“…We begin by reviewing the main ideas behind a Fisher analysis. For stationary and Gaussian noise, and in the large SNR limit, the posterior probability distribution of the template parameter vector θ a with a given signal s is approximately given by [92,93]…”

Section: Preliminarymentioning

confidence: 99%

“…with a tilde and * denoting the Fourier transform and complex conjugate operations respectively, and S n (f ) the noise spectral density. We follow [91][92][93] and consider a crude prior distribution on certain parameters, given by a Gaussian centered aroundθ a :…”

Section: Preliminarymentioning

confidence: 99%

Approximate universal relations among tidal parameters for neutron star binaries

Yagi

Yunes

2016

Class. Quantum Grav.

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One of largest uncertainties in nuclear physics is the relation between the pressure and density of supranuclear matter: the equation of state. Some of this uncertainty may be removed through future gravitational wave observations of neutron star binaries by extracting the tidal deformabilities (or Love numbers) of neutron stars, a novel way to probe nuclear physics in the high-density regime. Previous studies have shown that only a certain combination of the individual (quadrupolar) deformabilities of each body (the so-called chirp tidal deformability) can be measured with second-generation, gravitational wave interferometers, such as Adv. LIGO, due to correlations between the individual deformabilities. To overcome this, we search for approximately universal (i.e. approximately equation-of-state independent) relations between two combinations of the individual tidal deformabilities, such that once one of them has been measured, the other can be automatically obtained and the individual ones decoupled through these relations. We find an approximately universal relation between the symmetric and the anti-symmetric combination of the individual tidal deformabilities that is equation-of-state-insensitive to 20% for binaries with masses less than 1.7M . We show that these relations can be used to eliminate a combination of the tidal parameters from the list of model parameters, thus breaking degeneracies and improving the accuracy in parameter estimation. A simple (Fisher) study shows that the universal binary Love relations can improve the accuracy in the extraction of the symmetric combination of tidal parameters by as much as an order of magnitude, making the overall accuracy in the extraction of this parameter slightly better than that of the chirp tidal deformability. These new universal relations and the improved measurement accuracy on tidal parameters not only are important to astrophysics and nuclear physics, but also impact our ability to probe extreme gravity with gravitational waves and cosmology.Approximate Universal Relations among Tidal Parameters for NS Binaries * See e.g. [63][64][65][66][67][68][69][70] for other possibilities of probing cosmology with GW observations alone. † The signs of the terms proportional toλ a are opposite those in [46] because we use the convention m 1 ≤ m 2 (so thatλ a ≥ 0), while Ref.[46] used m 1 ≥ m 2 . ‡ The PN expansion is a series in powers of the ratio of the orbital velocity v of the binary to the speed of light c. A term of nPN order in a PN series corresponds to one that is of O[(v/c) 2n ] or equivalently O(x n ), relative to the leading order term in the series. * For rotating NSs, tidal effects enter first through their quadrupole moment, which appear at lower PN order than λ in the gravitational waveform. The effect of the quadrupole, however, is suppressed for * In [78], we show a similar figure for q = 0.75, in which one sees that the error bars for the stiff (soft) EoS classes decreases (increases) compared to those when q = 0.9. Thus, distinguishing betwe...

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Mixing and reaction efficiency in closed domains

Cited by 17 publications

References 26 publications

Dark Energy in Light of Multi-Messenger Gravitational-Wave Astronomy

Dark Energy in Light of Multi-Messenger Gravitational-Wave Astronomy

Bounding alternative theories of gravity with multiband GW observations

Approximate universal relations among tidal parameters for neutron star binaries

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