The Chemistry of Wet Surface Preparation

Tiec, Y. Le; Knotter, Martin

doi:10.1002/9781118578070.ch3

Cited by 4 publications

(3 citation statements)

References 37 publications

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“…Another extension would be to study the gravitational emission from a (stochastic) ensemble of small masses, such as brown dwarfs, in the case they are numerous around Sgr A*, or from dark matter clumps as mentioned in Sect. 5.7 (Le Tiec & et al 2019).…”

Section: Discussionmentioning

confidence: 99%

“…Weakly-interacting DM ( σv < 10 −30 cm 3 s −1 ) leads to an enclosed mass higher than 10 −4 M in the inner 10 M. Figure 6 shows that this leads to S/N 1 yr > 0.2, assuming that 10% inhomogeneities would appear in the DM distribution and orbit circularly around the MBH around 10 M. For nonannihilating DM, the S/N values can be as high as S/N 1 yr ∼ 10 4 . This makes a DM spike an interesting candidate for a potential gravitational wave source at the Galactic Center, to be studied in details in a forthcoming article (Le Tiec & et al 2019).…”

Section: Dark Mattermentioning

confidence: 99%

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Gravitational waves from bodies orbiting the Galactic center black hole and their detectability by LISA

Gourgoulhon

Tiec

Vincent

et al. 2019

A&A

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Aims. We present the first fully relativistic study of gravitational radiation from bodies in circular equatorial orbits around the massive black hole at the Galactic Center, Sgr A* and we assess the detectability of various kinds of objects by the gravitational wave detector LISA. Methods. Our computations are based on the theory of perturbations of the Kerr spacetime and take into account the Roche limit induced by tidal forces in the Kerr metric. The signal-to-noise ratio in the LISA detector, as well as the time spent in LISA band, are evaluated. We have implemented all the computational tools in an open-source SageMath package, within the Black Hole Perturbation Toolkit framework. Results. We find that white dwarfs, neutrons stars, stellar black holes, primordial black holes of mass larger than 10 −4 M , mainsequence stars of mass lower than ∼ 2.5 M , and brown dwarfs orbiting Sgr A* are all detectable in one year of LISA data with a signal-to-noise ratio above 10 for at least 10 5 years in the slow inspiral towards either the innermost stable circular orbit (compact objects) or the Roche limit (main-sequence stars and brown dwarfs). The longest times in-band, of the order of 10 6 years, are achieved for primordial black holes of mass ∼ 10 −3 M down to 10 −5 M , depending on the spin of Sgr A*, as well as for brown dwarfs, just followed by white dwarfs and low mass main-sequence stars. The long time in-band of these objects makes Sgr A* a valuable target for LISA. We also consider bodies on close circular orbits around the massive black hole in the nucleus of the nearby galaxy M32 and find that, among them, compact objects and brown dwarfs stay for 10 3 to 10 4 years in LISA band with a one-year signal-to-noise ratio above ten.

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Section: Discussionmentioning

confidence: 99%

Section: Dark Mattermentioning

confidence: 99%

Gravitational waves from bodies orbiting the Galactic center black hole and their detectability by LISA

Gourgoulhon

Tiec

Vincent

et al. 2019

A&A

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“…(5.6) of Ref. [115] and taking derivatives with respect to the components of the relative velocity [116], one gets…”

Section: Post-newtonian Expansionmentioning

confidence: 99%

Spin–orbit precession for eccentric black hole binaries at first order in the mass ratio

Akçay

Dempsey

Dolan

2017

Class. Quantum Grav.

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We consider spin-orbit ("geodetic") precession for a compact binary in strong-field gravity. Specifically, we compute ψ, the ratio of the accumulated spin-precession and orbital angles over one radial period, for a spinning compact body of mass m1 and spin s1, with s1 Gm 2 1 /c, orbiting a non-rotating black hole. We show that ψ can be computed for eccentric orbits in both the gravitational self-force and post-Newtonian frameworks, and that the results appear to be consistent. We present a post-Newtonian expansion for ψ at next-to-next-toleading order, and a Lorenz-gauge gravitational self-force calculation for ψ at first order in the mass ratio. The latter provides new numerical data in the strong-field regime to inform the Effective One-Body model of the gravitational two-body problem. We conclude that ψ complements the Detweiler redshift z as a key invariant quantity characterizing eccentric orbits in the gravitational two-body problem.

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Photovoltaic recycling: enhancing silicon wafer recovery process from damaged solar panels

Keerthivasan,

Madhesh,

Srinivasan

et al. 2024

J Mater Sci: Mater Electron

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The Chemistry of Wet Surface Preparation

Cited by 4 publications

References 37 publications

Gravitational waves from bodies orbiting the Galactic center black hole and their detectability by LISA

Gravitational waves from bodies orbiting the Galactic center black hole and their detectability by LISA

Spin–orbit precession for eccentric black hole binaries at first order in the mass ratio

Photovoltaic recycling: enhancing silicon wafer recovery process from damaged solar panels

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