Tilt interferometer for detecting gravitational wave signals at high frequencies

AbstractWe study gravitational wave (GW) production in strongly supercooled cosmological phase transitions, taking particular care of models featuring a complex scalar field with a U(1) symmetric potential. We perform lattice simulations of two-bubble collisions to properly model the scalar field gradients, and compute the GW spectrum sourced by them using the thin-wall approximation in many-bubble simulations. We find that in the U(1) symmetric case the low-frequency spectrum is $$\propto \omega $$ ∝ ω whereas for a real scalar field it is $$\propto \omega ^3$$ ∝ ω 3 . In both cases the spectrum decays as $$\omega ^{-2}$$ ω - 2 at high frequencies.

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Measuring the scalar induced gravitational waves from observations

The European Physical Journal C ◽

10.1140/epjc/s10052-021-09405-0 ◽

2021 ◽

Vol 81 (7) ◽

Author(s):

Jun Li ◽

Guang-Hai Guo

Keyword(s):

Power Spectrum ◽

Cosmic Microwave Background ◽

Gravitational Wave ◽

Gravitational Waves ◽

Cosmological Parameters ◽

Numerical Results ◽

Microwave Background ◽

High Frequencies ◽

Special Cases ◽

Relic Density

AbstractWe consider the scalar induced gravitational waves from the cosmic microwave background (CMB) observations and the gravitational wave observations. In the $$\Lambda $$ Λ CDM+r model, we constrain the cosmological parameters within the evolution of the scalar induced gravitational waves by the additional scalar power spectrum. The two special cases called narrow power spectrum and wide power spectrum have influence on the cosmological parameters, especially the combinations of Planck18+BAO+BK15+LISA. We also compare these numerical results from four datasets within LIGO, LISA, IPTA and FAST projects, respectively. The constraints from FAST have a significant impact on tensor-to-scalar ratio. Besides, we only consider the relic density of induced gravitational waves with respect to different frequencies from CMB scale to high frequencies including the range of LIGO and LISA.

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Higher-order geodesic deviation for charged particles and resonance induced by gravitational waves

International Journal of Modern Physics D ◽

10.1142/s0218271818500426 ◽

2018 ◽

Vol 27 (04) ◽

pp. 1850042 ◽

Cited By ~ 2

Author(s):

M. Heydari-Fard ◽

S. N. Hasani

Keyword(s):

Magnetic Field ◽

Magnetic Resonance ◽

Gravitational Wave ◽

Gravitational Waves ◽

Constant Magnetic Field ◽

Charged Particles ◽

Higher Order ◽

Geodesic Deviation ◽

High Frequencies ◽

Test Particles

We generalize the higher-order geodesic deviation for the structure-less test particles to the higher-order geodesic deviation equations of the charged particles [R. Kerner, J. W. van Holten and R. Colistete Jr., Class. Quantum Grav. 18 (2001) 4725]. By solving these equations for charged particles moving in a constant magnetic field in the spacetime of a gravitational wave, we show for both cases when the gravitational wave is parallel and perpendicular to the constant magnetic field, a magnetic resonance appears at [Formula: see text]. This feature might be useful to detect the gravitational wave with high frequencies.

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Quasi-Periodic Oscillations in Dwarf Novae

International Astronomical Union Colloquium ◽

10.1017/s0252921100073310 ◽

1979 ◽

Vol 46 ◽

pp. 77-88

Author(s):

Edward L. Robinson

Keyword(s):

Binary Systems ◽

Outer Edge ◽

Light Curves ◽

Close Binary ◽

Bright Spot ◽

Dwarf Novae ◽

Periodic Oscillations ◽

High Frequencies ◽

Short Period ◽

Typical Time

Three distinct kinds of rapid variations have been detected in the light curves of dwarf novae: rapid flickering, short period coherent oscillations, and quasi-periodic oscillations. The rapid flickering is seen in the light curves of most, if not all, dwarf novae, and is especially apparent during minimum light between eruptions. The flickering has a typical time scale of a few minutes or less and a typical amplitude of about .1 mag. The flickering is completely random and unpredictable; the power spectrum of flickering shows only a slow decrease from low to high frequencies. The observations of U Gem by Warner and Nather (1971) showed conclusively that most of the flickering is produced by variations in the luminosity of the bright spot near the outer edge of the accretion disk around the white dwarf in these close binary systems.

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