Scientific Potential of Decigo Pathfinder and Testing Gr With Space-Borne Gravitational Wave Interferometers

Yagi, Kent

doi:10.1142/s0218271813410137

Cited by 64 publications

(61 citation statements)

References 412 publications

(507 reference statements)

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“…The most sensitive experiment in this observational window is the Big Bang observer (BBO), a proposed fourth-generation space based interferometer experiment, in a hexagram configuration [61][62][63]. The Deci-Hertz Interferometer Gravitational Wave Observatory (DECIGO) is a space-based Fabry-Perot interferometer which was proposed as early as 2001 [64,70]. B-DECIGO [65] is the scaled-down version of DECIGO (the B stands for "basic").…”

Section: (315)mentioning

confidence: 99%

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Dynamical axions and gravitational waves

Croon

Houtz

Sanz

2019

J. High Energ. Phys.

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In this paper we explore the possibility of observable gravitational waves as a manifestation of the QCD axion dynamics. In particular, we focus on dynamical axion models which solve the strong CP problem, and include the confinement of a QCD-like gauge group at the TeV scale. We study the resulting chiral symmetry breaking phase transition for models with N F = 3 and N F = 4 light flavors using the linear sigma model. This model describes the scalar meson spectrum and its interactions, with the diagonal field ϕ as the order parameter. We find that the amplitude of the gravitational wave spectrum depends on the mass of the dynamical axion η via the ratio m η /m ϕ . The resulting spectra may be observed at future mid-range gravitational wave experiments such as AION/MAGIS, DECIGO, and BBO. Moreover, the TeV states can be searched for at colliders and their quantum numbers characterized, providing a unique connection between axion physics, gravitational waves and collider searches.

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Section: (315)mentioning

confidence: 99%

“…For clarity, the peaks of the spectra are indicated with a point. The experimental projections for the Big Bang Observer (BBO)[61][62][63], Fabry-Perot DECIGO (original proposal)[64], B-DECIGO (scaled-down version)[65], and MAGIS-AION (space-born)[66][67][68] are plotted.…”

mentioning

confidence: 99%

Dynamical axions and gravitational waves

Croon

Houtz

Sanz

2019

J. High Energ. Phys.

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“…WD binaries, especially those observed as AM CVn-stars and ultracompact X-ray binaries (UCXB), are potential GW sources within the frequency band (10 −4 − 1) Hz of the space GW interferometers like (the currently cancelled) LISA [187],1 NGO (eLISA) [10, 11], DEGIGO [857] and other proposed or planned low-frequency GW detectors [122, 40]. At the moment, eLISA is selected for the third large-class mission in ESA’s Cosmic Vision science program (L3).…”

Section: Introductionmentioning

confidence: 99%

The Evolution of Compact Binary Star Systems

Постнов

Yungelson

2014

Living Rev. Relativ.

453

382

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We review the formation and evolution of compact binary stars consisting of white dwarfs (WDs), neutron stars (NSs), and black holes (BHs). Mergings of compact-star binaries are expected to be the most important sources for forthcoming gravitational-wave (GW) astronomy. In the first part of the review, we discuss observational manifestations of close binaries with NS and/or BH components and their merger rate, crucial points in the formation and evolution of compact stars in binary systems, including the treatment of the natal kicks, which NSs and BHs acquire during the core collapse of massive stars and the common envelope phase of binary evolution, which are most relevant to the merging rates of NS-NS, NS-BH and BH-BH binaries. The second part of the review is devoted mainly to the formation and evolution of binary WDs and their observational manifestations, including their role as progenitors of cosmologically-important thermonuclear SN Ia. We also consider AM CVn-stars, which are thought to be the best verification binary GW sources for future low-frequency GW space interferometers.

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“…As such, the study of these binaries provides important input to programs to solve the two-body problem of general relativity more generally, such as numerical relativity and the effective one-body approach [1][2][3] . Second, astrophysical extreme mass ratio inspirals (EMRIs) are expected to be important sources for space-based GW detectors such as eLISA 4 and DECIGO 5 . In this article, we will focus on the role of EMRIs as sources of gravitational waves (GWs).…”

Section: Motivation: the Large-mass Ratio Limit Of The Two-body Problmentioning

confidence: 99%

Adiabatic and post-adiabatic approaches to extreme mass ratio inspiral

Hughes¹

2017

The Fourteenth Marcel Grossmann Meeting

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Extreme mass ratio inspirals (EMRIs) show a strong separation of timescales, with the time characterizing inspiral, T i , much longer than any time To characterizing orbital motions. The ratio of these timescales (which is essentially an EMRI's mass ratio) can be regarded as a parameter that controls a perturbative expansion. Here we describe the value and limitations of an "adiabatic" description of these binaries, which uses only the leading terms arising from such a two-timescale expansion. An adiabatic approach breaks down when orbits evolve through resonances, with important dynamical and observational consequences. We describe the shortfalls of an approach that only includes the adiabatic contributions to EMRI evolution, and outline what must be done to evolve these systems through resonance and to improve our ability to model EMRI systems more generally.Keywords: Black holes; black hole perturbation theory; gravitational waves. Motivation: The large-mass ratio limit of the two-body problem and extreme mass ratio inspiralsBinary systems in which one body is much more massive than the other can be analyzed perturbatively. We can describe such a binary as an exact black hole solution of general relativity (corresponding to the larger member of the binary) plus a correction due to the smaller body. Because the perturbation equations are much simpler to solve than the complete equations of general relativity, this turns out to be a limit that can be modeled very accurately and precisely. At least two major science goals drive studies of large mass ratio systems. First, these binaries represent a limit of the two-body problem that can be solved with high precision. As such, the study of these binaries provides important input to programs to solve the two-body problem of general relativity more generally, such as numerical relativity and the effective one-body approach 1-3 . Second, astrophysical extreme mass ratio inspirals (EMRIs) are expected to be important sources for space-based GW detectors such as eLISA 4 and DECIGO 5 . In this article, we will focus on the role of EMRIs as sources of gravitational waves (GWs). Such binaries are created when multibody interactions scatter stellar mass compact objects onto a strong-field, relativistic orbit of the black hole in a galaxy's center. Further evolution is then driven by GW emission. If the black hole has a mass of around 10 5 − 10 7 M , then these are targets for a detector like eLISA. The GWs that they generate can be heard out to z ∼ 0.5 − 1; we expect dozens to hundreds of events over a space-based detector's mission lifetime 6 . Measuring the GWs from these events will provide precision data on the characteristics of the large black hole, on the small body's orbit, and on the mass of the small bodyin short, a precision probe of the astrophysical population of galactic center black

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Scientific Potential of Decigo Pathfinder and Testing Gr With Space-Borne Gravitational Wave Interferometers

Cited by 64 publications

References 412 publications

Dynamical axions and gravitational waves

Dynamical axions and gravitational waves

The Evolution of Compact Binary Star Systems

Adiabatic and post-adiabatic approaches to extreme mass ratio inspiral

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