High‐Frequency Gravitational Waves in Electromagnetic Waveguides

Sorge, Francesco

doi:10.1002/andp.202300228

Annalen der Physik

2023

DOI: 10.1002/andp.202300228

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High‐Frequency Gravitational Waves in Electromagnetic Waveguides

Francesco Sorge

Abstract: The interaction between a very‐high‐frequency gravitational wave (VHFGW) and an electromagnetic wave (EMW) in a rectangular waveguide is discussed in the weak field limit. The background EMW is assumed to be initially in the TE10 mode along the waveguide. It is then shown that a VHFGW, having the same frequency and direction of propagation of the EMW, induces through the waveguide a TE mode with a frequency doubled when compared to the original EMW frequency. In that respect, the GW acts similar to a non‐linea… Show more

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2024

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Cited by 3 publications

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A coordinate-independent formalism for detecting high-frequency gravitational waves

Ratzinger,

Schenk,

Schwaller

2024

J. High Energ. Phys.

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In an external electric or magnetic field, a gravitational wave (GW) may be converted into electromagnetic radiation. We present a coordinate-invariant framework to describe the GW signal in a detector that is based on this effect, such as cavities for axion searches. In this framework, we pay special attention to the definition of manifestly coordinate-independent expressions for the electromagnetic fields that an external observer would detect. A careful assessment of the detector’s perceived motion allows us to treat both its mechanical and its electromagnetic response to the GW consistently. We further introduce well-defined approximations for which this motion may be neglected, and hence provide suggestions on which coordinate frame is suitable to characterise the GW signal in practice. We illustrate our findings in two examples, an infinitesimally thin rod and a spherical electromagnetic cavity.

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A coordinate-independent formalism for detecting high-frequency gravitational waves

Ratzinger,

Schenk,

Schwaller

2024

J. High Energ. Phys.

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Ultrahigh frequency primordial gravitational waves beyond the kHz: The case of cosmic strings

Servant,

Simakachorn

2024

Phys. Rev. D

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We investigate gravitational-wave backgrounds (GWBs) of primordial origin that would manifest only at ultrahigh frequencies, from kilohertz to 100 gigahertz, and leave no signal at LIGO, the Einstein Telescope, the Cosmic Explorer, LISA, or pulsar-timing arrays. We focus on GWBs produced by cosmic strings and make predictions for the GW spectra scanning over high-energy scale (beyond 1010 GeV) particle physics parameters. Signals from local string networks can easily be as large as the big bang nucleosynthesis/cosmic microwave background bounds, with a characteristic strain as high as 10−26 in the 10 kHz band, offering prospects to probe grand unification physics in the 1014–1017 GeV energy range. In comparison, GWB from axionic strings is suppressed (with maximal characteristic strain ∼10−31) due to the early matter era induced by the associated heavy axions. We estimate the needed reach of hypothetical futuristic GW detectors to probe such GWB and, therefore, the corresponding high-energy physics processes. Beyond the information of the symmetry-breaking scale, the high-frequency spectrum encodes the microscopic structure of the strings through the position of the UV cutoffs associated with cusps and kinks, as well as potential information about friction forces on the string. The IR slope, on the other hand, reflects the physics responsible for the decay of the string network. We discuss possible strategies for reconstructing the scalar potential, particularly the scalar self-coupling, from the measurement of the UV cutoff of the GW spectrum. Published by the American Physical Society 2024

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Enhanced primordial gravitational waves from a stiff postinflationary era due to an oscillating inflaton

Chen,

Dimopoulos,

Eröncel

et al. 2024

Phys. Rev. D

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We investigate two classes of inflationary models, which lead to a stiff period after inflation that boosts the signal of primordial gravitational waves (GWs). In both families of models studied, we consider an oscillating scalar condensate, which when far away from the minimum is overdamped by a warped kinetic term, la α-attractors. This leads to successful inflation. The oscillating condensate is in danger of becoming fragmented by resonant effects when nonlinearities take over. Consequently, the stiff phase cannot be prolonged enough to enhance primordial GWs at frequencies observable in the near future for low orders of the envisaged scalar potential. However, this is not the case for a higher-order scalar potential. Indeed, we show that this case results in a boosted GW spectrum that overlaps with future observations without generating too much GW radiation to destabilize big bang nucleosynthesis. For example, taking α=O(1), we find that the GW signal can be safely enhanced up to ΩGW(f)∼10−11 at frequency f∼102 Hz, which will be observable by the Einstein Telescope. Our mechanism ends up with a characteristic GW spectrum, which if observed, can lead to the determination of the inflation energy scale, the reheating temperature, and the shape (steepness) of the scalar potential around the minimum. Published by the American Physical Society 2024

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High‐Frequency Gravitational Waves in Electromagnetic Waveguides

Cited by 3 publications

References 27 publications

A coordinate-independent formalism for detecting high-frequency gravitational waves

A coordinate-independent formalism for detecting high-frequency gravitational waves

Ultrahigh frequency primordial gravitational waves beyond the kHz: The case of cosmic strings

Enhanced primordial gravitational waves from a stiff postinflationary era due to an oscillating inflaton

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