Searching for Mini Extreme Mass Ratio Inspirals with Gravitational-Wave Detectors

Guo, Huai-Ke; Miller, Andrew H.

doi:10.48550/arxiv.2205.10359

Cited by 6 publications

(5 citation statements)

References 82 publications

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“…Finally, if the third body is assumed to be a NS, its mass needs to be at least around the Chandrasekhar threshold mass of m 3 ∼ 1.4M ⊙ , which due to the asymmetry constraints leads to the conclusion that m 1 ≳ 10 3 M ⊙ , a BH mass range that current detectors have not been able to access so far, but that further observation runs of LVK detectors [37] or the third generation detectors like ET [38] can in principle probe. Moreover, if we consider the scenario in which the binary is formed by two supermassive black holes [39] or the combination of a supermassive and an intermediate-mass black holes [40], then the third body could be a black hole with a mass anywhere in the range m 3 ∈ [1.4, 100]M ⊙ .…”

Section: Discussionmentioning

confidence: 99%

Gravitational waves in the circular restricted three body problem

Martin Barandiaran,

Kuroyanagi,

Nesseris

2024

Class. Quantum Grav.

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The prospect of unprecedented high-quality data of gravitational waves in the upcoming decades demands a theoretical effort to optimally study and analyze the signals that next generation detectors will provide. Here we study the gravitational wave emission and related dynamics during the inspiralling phase of the Circular Restricted Three Body Problem, a modification of the conventional binary scenario in which a small third object co-rotates with the parent binary system. Specifically, we obtain analytic expressions for the emitted power, frequency variation and other dynamical variables that describe the evolution of the system. As a key highlight, we find that the presence of the third body actually slows down the coalescence of the binary, which can be partially interpreted as an effective rescaling of the binary's chirp-mass. Our analysis assumes semi-Keplerian orbits for the particles and a highly mass asymmetric parent binary needed for the stability of orbits.

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Section: Discussionmentioning

confidence: 99%

Gravitational waves in the circular restricted three body problem

Martin Barandiaran,

Kuroyanagi,

Nesseris

2024

Class. Quantum Grav.

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“…Indeed, the GW signals emitted by these systems, when the two compact objects are far away from the coalescence and their masses are small enough, say < 10 −2 M , i.e below the mass range considered in section 6.3.3, can be modeled as CW or tCW signals with a spin-up described by a power law, see e.g. [440,511].…”

Section: Jcap07(2023)068mentioning

confidence: 99%

Science with the Einstein Telescope: a comparison of different designs

Branchesi¹,

Maggiore²,

Alonso³

et al. 2023

J. Cosmol. Astropart. Phys.

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The Einstein Telescope (ET), the European project for a third-generation gravitational-wave detector, has a reference configuration based on a triangular shape consisting of three nested detectors with 10 km arms, where each detector has a 'xylophone' configuration made of an interferometer tuned toward high frequencies, and an interferometer tuned toward low frequencies and working at cryogenic temperature. Here, we examine the scientific perspectives under possible variations of this reference design. We perform a detailed evaluation of the science case for a single triangular geometry observatory, and we compare it with the results obtained for a network of two L-shaped detectors (either parallel or misaligned) located in Europe, considering different choices of arm-length for both the triangle and the 2L geometries. We also study how the science output changes in the absence of the low-frequency instrument, both for the triangle and the 2L configurations. We examine a broad class of simple 'metrics' that quantify the science output, related to compact binary coalescences, multi-messenger astronomy and stochastic backgrounds, and we then examine the impact of different detector designs on a more specific set of scientific objectives.

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“…Very light ( < ∼ O(10 −10 M −10 −3 M )) PBH binaries would generate long-lived GWs during inspiraling, lasting at least O(hours-days) and potentially up to thousands or million years. A method has been designed to search for these GWs [479], and those from mini-EMRI ones [480], with constraints placed using upper limits from searching for quasi-monochromatic, persistent GWs in O3 from planetary and asteroid-mass PBHs [481,482]. CE and ET could even detect such binaries in the solar system vicinity.…”

Section: Bh Mergers At High Redshift the Third Generation Of Gw Detec...mentioning

confidence: 99%

Detection of early-universe gravitational-wave signatures and fundamental physics

et al. 2022

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Detection of a gravitational-wave signal of non-astrophysical origin would be a landmark discovery, potentially providing a significant clue to some of our most basic, big-picture scientific questions about the Universe. In this white paper, we survey the leading early-Universe mechanisms that may produce a detectable signal—including inflation, phase transitions, topological defects, as well as primordial black holes—and highlight the connections to fundamental physics. We review the complementarity with collider searches for new physics, and multimessenger probes of the large-scale structure of the Universe.

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Searching for Mini Extreme Mass Ratio Inspirals with Gravitational-Wave Detectors

Cited by 6 publications

References 82 publications

Gravitational waves in the circular restricted three body problem

Gravitational waves in the circular restricted three body problem

Science with the Einstein Telescope: a comparison of different designs

Detection of early-universe gravitational-wave signatures and fundamental physics

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