REVIEW 3 major objections 4 minor 134 references
Kination-like Era Driven by the Effective Inflaton/Higgs Potential
T0 review · 3 major / 4 minor · reviewed 2026-08-15 · deepseek-v4-flash
Pith's one-line read The paper claims that radiative corrections to the U(1)_X Higgs inflaton potential generate a stiff post-inflationary era whose gradually changing equation of state bends the primordial gravitational-wave spectrum into a curved…
desk verdict Sound model-specific application of the known stiff-era GW mechanism to minimal U(1)_X inflation with concrete benchmarks and a collider link, but the detectability claims rest on an unexamined preheating assumption. read the letter →
The pith
A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.
The reading
What carries the argument
The load-bearing object is the Coleman-Weinberg effective potential of the U(1)_X Higgs field, Eq. (7): $V_{\rm eff}\simeq \frac14\left(\lambda_\phi+\frac{\beta_\lambda}{2}\ln\frac{\phi^2}{\phi_{\min}^2}\right)\phi^4-\frac14\lambda_\phi\phi_{\min}^4$, with $\beta_\lambda=96g_X^4/(16\pi^2)$. The identity that turns this into a stiff era is the virial result for an oscillating scalar in a power-law potential $V\propto\phi^p$: the time-averaged equation of state is $w=(p-2)/(p+2)$, so any potential steeper than $\phi^4$ gives $w>1/3$, and the logarithm in the effective potential makes the local slope $p(\phi)$ grow with oscillation amplitude. The paper's semi-analytic calculation connects this slope to the averaged equation of state as a function of scale factor, and the gravitational-wave transfer function of Eq. (13) maps each mode's horizon re-entry during the era of varying $w$ onto the present-day spectrum, producing the curved enhancement. A non-minimal coupling $\xi\phi^2 R$ flattens the potential during inflation, and the analysis assumes this coupling is negligible once oscillation begins, so the tree-level quartic regime is replaced by the radiatively steeper form.
What would settle it
A numerical lattice simulation of preheating in this model, starting at the end of inflation with the Coleman-Weinberg potential and $g_X\simeq 0.016$, would settle the central claim: if it shows the inflaton amplitude decaying by parametric resonance before $w$ pulls above $1/3$, the kination era and the enhanced gravitational-wave spectrum do not occur. Observationally, a flat rather than curved inflationary gravitational-wave spectrum at the frequencies mapped to the stiff era would also rule out the benchmark scenario.
Extended reading notes
Core claim
Identifying the U(1)_X Higgs field $\Phi$ with the inflaton, the paper starts from a classically conformal U(1)_X sector in which the quartic self-coupling is negligible compared to the gauge coupling $g_X$. Radiative corrections then give the one-loop Coleman-Weinberg potential, $V_{\rm eff}\simeq \frac{1}{4}\left(\lambda_\phi+\frac{\beta_\lambda}{2}\ln\frac{\phi^2}{\phi_{\min}^2}\right)\phi^4-\frac{1}{4}\lambda_\phi\phi_{\min}^4$ with $\beta_\lambda=96g_X^4/(16\pi^2)$, which is steeper than the quartic $\phi^4$ potential at large amplitude. Since an oscillating scalar in a potential $V\propto\phi^p$ has average equation of state $w=(p-2)/(p+2)$, the logarithmic steepening pushes $w$ above $1/3$ during the early post-inflation oscillation, producing a kination-like era that persists until the amplitude drops near the minimum, after which a matter-dominated era precedes reheating. The paper's semi-analytic calculation represents this by a slowly varying exponent $p(\phi)$ and reproduces the numerically averaged $w$ to good accuracy. Feeding this time-dependent $w$ into the gravitational-wave transfer function yields a curved spectrum: flat at low frequencies, rising with a gradually increasing tilt over modes that re-enter during the stiff era, falling during matter domination, and cut off at the high-frequency end, with the whole shape fixed by $g_X$ and $M_{Z'}$.
Load-bearing premise
The central premise is that the inflaton keeps oscillating coherently along the Coleman-Weinberg potential, without preheating or particle production draining its energy, through the entire amplitude range that produces $w>1/3$; if that coherence fails, the stiff era is shortened or absent and the gravitational-wave enhancement is overestimated.
Editorial extensions
If this is right
- The inflationary stochastic gravitational-wave background is not necessarily scale-invariant: a steeper-than-quartic oscillating scalar produces a stiff era whose imprint is a rising, curved segment in $\Omega_{\rm GW}(f)$ between the low-frequency flat part and the matter-dominated fall.
- Within this model, once the non-minimal coupling, the inflaton vacuum expectation value and the e-folding number are fixed, the gauge coupling $g_X$ and the Z' mass $M_{Z'}=2g_X\phi_{\min}$ are determined; benchmark points with $M_{Z'}\sim 1.6$ TeV give an enhanced spectrum overlapping U-DECIGO while the same Z' is accessible to hadron-collider dilepton searches.
- Benchmarks with very large $M_{Z'}$ (around $5\times 10^7$ GeV) move the enhancement to high frequencies, giving ultra-high-frequency gravitational-wave detectors a concrete target that colliders cannot reach.
- Because $w$ grows gradually rather than staying constant during the kination-like phase, the resulting spectrum is curved rather than a single power law, offering a way to distinguish this radiative-potential origin from other stiff-era scenarios.
Reading between the lines
- The paper leaves implicit that the same mechanism generalizes to any classically conformal scalar with a radiative effective potential; the slope of the curved gravitational-wave spectrum would then encode the beta-function coefficient of the relevant gauge group, effectively turning the spectrum into a particle-physics measurement.
- An unaddressed risk is preheating: because the inflaton is coupled to the U(1)_X gauge field, parametric resonance could transfer the condensate's energy into Z' bosons before the amplitude drops to the small-amplitude regime, shortening or erasing the stiff era; a lattice simulation of this preheating would test whether the enhanced spectra survive.
- A natural cross-check is to integrate the gravitational-wave mode equation through the continuous $w(a)$ evolution rather than approximating the era by piecewise-constant equations of state, which would show whether the curved features of the predicted spectra are robust in detail.
Signed reviews
Editorial analysis
A structured set of objections, weighed in public.
Referee Report
Summary. This paper proposes that in the minimal U(1)_X extension of the Standard Model, the U(1)_X Higgs field serving as the inflaton can yield a kination-like phase (w > 1/3) after inflation because the Coleman-Weinberg effective potential is slightly steeper than phi^4. This stiff phase modulates and amplifies the inflationary stochastic gravitational wave background in a characteristic frequency band. The authors develop a semi-analytic calculation of the post-inflationary equation of state, validate it against a toy numerical model, and present benchmark points for which the resulting GW spectrum is detectable by future experiments such as U-DECIGO. They also interpret the ATLAS dilepton resonance search to constrain the U(1)_X charge parameter x_H for a benchmark point, illustrating complementarity between GW observations and collider searches.
Significance. The paper offers a concrete, UV-motivated scenario in which a stiff post-inflationary era emerges from the particle physics model itself rather than being put in by hand. The central physical argument that a potential steeper than phi^4 gives w > 1/3 is correct, and the semi-analytic method is a useful tool. The predicted spectrum has a distinct curved shape that could, in principle, be distinguished from constant-w kination scenarios. The collider complementarity is a nice addition. However, the robustness of the prediction is not yet established, because the preheating dynamics and the inflaton decay rate, which set the duration of the stiff era, are not analyzed. The paper's potential also contains a sign inconsistency in the stationary condition that needs to be corrected.
major comments (3)
- [Sec. III B–III C] The central assumption that the inflaton oscillates coherently without particle production is not justified. The U(1)_X Higgs inflaton has a gauge coupling g_X to the Z' boson, whose mass m_Z'(t) = 2 g_X phi(t) oscillates with the inflaton. For the benchmark values (g_X ~ 0.016 and effective quartic lambda_eff ~ 1e-6 at the amplitudes reached just after inflation), the adiabaticity ratio m_Z'/omega_osc ~ 2 g_X / sqrt(lambda_eff) is of order tens, which is the regime of efficient broad parametric resonance. If the gauge field modes grow faster than H, the condensate is destroyed before the amplitude enters the region where w rises appreciably above 1/3, and the kination-like era is shortened or absent. The numerical validation in Fig. 1 is a single-field toy model and cannot capture this channel. Please add a preheating analysis (Floquet indices or lattice simulation) for the benchmark points, or provide a concrete reason why particle production is ineffective.
- [Sec. III C] The treatment of reheating is internally inconsistent. The text calls T_rh 'essentially a free parameter' in Sec. III C, but Sec. V states that the reheating temperature is 'fixed in a consistent manner.' In the calculation, T_rh is fixed by Eq. (12) through the matching of the CMB pivot scale, but Eq. (12) only enforces the e-fold budget; it does not compute the inflaton decay width, which is the physical quantity that determines T_rh. The decay width involves the same couplings (g_X and y_M) that also control preheating, so a self-consistent treatment is required. Please clarify whether T_rh is an input or an output, and if it is an output, provide the decay width calculation; if it is an input, vary it to demonstrate how the GW spectrum changes.
- [Eq. (7) and Sec. III B] The stationary condition for the Coleman-Weinberg potential is stated incorrectly. Differentiating Eq. (7) with respect to phi and setting phi = phi_min gives dV/dphi|_{phi_min} = (lambda_phi + beta_lambda/4) phi_min^3, so the condition dV/dphi = 0 yields lambda_phi = -beta_lambda/4, not lambda_phi = beta_lambda/4 as stated. This sign error propagates to the relation between g_X and the inflationary potential and to the benchmark points in Table II. Please verify the coefficients of the effective potential and the resulting relation between lambda_phi and g_X.
minor comments (4)
- [After Eq. (13)] The sentence 'After the reheating is complete at a_rh, w_avg becomes 0' should presumably read 'w_avg becomes 1/3,' since the flat spectrum to the left of k_rh corresponds to radiation domination.
- [Eq. (12)] The e-fold matching equation is difficult to parse because of the ambiguous ellipsis and the product structure. Please rewrite the equation and define each ratio explicitly so that the reader can follow how T_rh is obtained.
- [Sec. V] The statement that the inflaton potential is controlled by only two free parameters (xi and phi_min) conflicts with Table II, where N_inf is also an input; please clarify the parameter counting.
- [Footnote 2] The word 'unegligible' appears to be a typo; the intended word is likely 'negligible.'
Circularity Check
No significant circularity: the stiff-era EOS and GW modulation follow from the Coleman-Weinberg potential and are not fitted to GW data.
full rationale
The derivation is self-contained. Equation (7) defines the one-loop Coleman-Weinberg potential with beta_lambda fixed by g_X, and the stationary condition fixes lambda_phi = beta_lambda/4. The stiff-era EOS w > 1/3 follows from the standard virial result w = (p-2)/(p+2) applied to the local power index p(phi) = d(log V)/d(log phi) of this potential, and the semi-analytic calculation is validated against a numerical single-field toy in Fig. 1. The value of g_X is fixed by CMB normalization through the non-minimally coupled quartic tree-level potential; M_Z' = 2 g_X phi_min and T_rh are then derived, with T_rh obtained from the scale-factor consistency relation in Eq. (12), rather than adjusted to reproduce the GW spectrum. The benchmark GW spectra in Fig. 2 are forward-modeled outputs from the chosen inputs (xi, phi_min, N_inf) and are not fitted to any GW observation. Self-citations (e.g., Refs. [14,15,17]) appear only as background for the known stiff-era enhancement of inflationary gravitational waves and are not load-bearing for the CW-potential computation. The preheating concern raised by the reader is a physical robustness or correctness issue, not a circularity; no equation in the paper defines a predicted quantity in terms of itself or renames a fitted parameter as a prediction.
Assumptions & free parameters
free parameters (5)
- xi (non-minimal gravitational coupling) =
100 for all benchmark points
- phi_min (U(1)_X Higgs VEV) =
1.6e9 GeV (BM1, BM3); 5e4 GeV (BM2, BM4)
- N_inf (e-foldings) =
55, 55, 55.6, 55.3 for BM1 to BM4
- T_rh (reheating temperature) =
1.11e7, 141.31, 2.15e7, 534.74 GeV for BM1 to BM4
- x_H (U(1)_X charge parameter) =
constrained to -1.57 < x_H < -0.434 by ATLAS for BM4
assumptions (7)
- standard math The minimal U(1)_X model with three right-handed neutrinos is anomaly-free and provides the seesaw mechanism.
- ad hoc to paper The U(1)_X Higgs sector is classically conformal, with a massless renormalization condition at phi = 0 and lambda_phi, |y_N|^2 << g_X^2.
- domain assumption The mixed quartic coupling lambda_mix between the SM and U(1)_X Higgs fields is negligible.
- domain assumption Kinetic mixing between U(1)_Y and U(1)_X gauge bosons is neglected; the RG flow is at most a few percent.
- ad hoc to paper No efficient preheating or parametric resonance occurs while the inflaton oscillates; energy density stays in the homogeneous field until EMD.
- domain assumption Inflaton decay is perturbative and can realize any reheating temperature used in Eq. (12).
- domain assumption The primordial tensor spectrum is scale-invariant and the transfer through piecewise-constant EOS phases is valid.
Cite this review
Pith. "Pith review of Kination-like Era Driven by the Effective Inflaton/Higgs Potential." pith.science (2026). https://pith.science/paper/B2SIYMKH
@misc{pith2026250508786,
author = {Pith},
title = {Pith review of: Kination-like Era Driven by the Effective Inflaton/Higgs Potential},
year = {2026},
howpublished = {\url{https://pith.science/paper/B2SIYMKH}},
note = {Machine review of arXiv:2505.08786}
}
abstract
Based on the minimal $U(1)_X$ extended Standard Model, we explore cosmic inflation where the $U(1)_X$ Higgs field serves as the inflaton. We demonstrate that a stiff era with an equation of state $w > 1/3$ can emerge during the inflaton's oscillatory phase after inflation, driven by the Coleman-Weinberg potential of the inflaton, arising due to radiative corrections. This leads to significant modulation and enhancement of the irreducible stochastic gravitational wave (GW) background from inflation, deviating from the conventional scale-invariant spectrum. Such a distinct GW spectrum could be detectable by next-generation GW interferometer missions, such as U-DECIGO. In our framework, the GW spectrum depends on the $U(1)_X$ gauge coupling and the mass of the $U(1)_X$ gauge boson ($Z^\prime$). As a result, future GW observations and $Z^\prime$ boson resonance searches at high-energy collider experiments are complementary to one another.
Figures
Reference graph
Works this paper leans on
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[1]
Numerical Study with a Toy Model Given a potential, we can understand the dynamics of the inflaton by solving its equation of motion (EOM): ¨φ + 3H ˙φ +V,φ = 0, (8) where the dot denotes derivative with respect to cosmic time t, H = ˙a/a is the Hubble pa- rameter with a being the scale factor of the Friedmann-Lemaitre-Robertson-Walker metric, 7 and V,φ = ...
-
[2]
Toward a simpler but sufficiently accurate calculations, we develop a semi-analytic calculation (SAC) in this section
Semi-Analytic Calculations For the effective potential, solving the EOM from the inflation era to the oscillation era to evaluatew(t) is numerically difficult. Toward a simpler but sufficiently accurate calculations, we develop a semi-analytic calculation (SAC) in this section. As mentioned in the previous subsection, we calculate w(t) as an average over ...
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[3]
This lets us find arh and hence Trh from eq.12, thereby fixing the duration of EMD phase. IV. GRAVITATIONAL WAVE AND COLLIDER SIGNATURES A. Modulated GW spectrum The GW spectrum produced during the inflation is flat (scale-invariant). However, when the modes of the GW reenter the horizon during different epochs with different EOSs, the flat GW spectrum ge...
2019
-
[4]
The Creation of the Universe as a Quantum Phenomenon,
R. Brout, F. Englert, and E. Gunzig, “The Creation of the Universe as a Quantum Phenomenon,” Annals Phys. 115 (1978) 78
1978
-
[5]
First Order Phase Transition of a Vacuum and Expansion of the Universe,
K. Sato, “First Order Phase Transition of a Vacuum and Expansion of the Universe,” Mon. Not. Roy. Astron. Soc. 195 (1981) 467–479
1981
-
[6]
The Inflationary Universe: A Possible Solution to the Horizon and Flatness Problems,
A. H. Guth, “The Inflationary Universe: A Possible Solution to the Horizon and Flatness Problems,” Phys. Rev. D 23 (1981) 347–356
1981
-
[7]
A New Inflationary Universe Scenario: A Possible Solution of the Horizon, Flatness, Homogeneity, Isotropy and Primordial Monopole Problems,
A. D. Linde, “A New Inflationary Universe Scenario: A Possible Solution of the Horizon, Flatness, Homogeneity, Isotropy and Primordial Monopole Problems,” Phys. Lett. B 108 (1982) 389–393
1982
-
[8]
Dynamics of Phase Transition in the New Inflationary Universe Scenario and Generation of Perturbations,
A. A. Starobinsky, “Dynamics of Phase Transition in the New Inflationary Universe Scenario and Generation of Perturbations,” Phys. Lett. B 117 (1982) 175–178
1982
Show all 134 references
-
[9]
Planck 2018 results. VI. Cosmological parameters,
Planck Collaboration, N. Aghanim et al., “Planck 2018 results. VI. Cosmological parameters,” Astron. Astrophys. 641 (2020) A6, arXiv:1807.06209 [astro-ph.CO] . [Erratum: Astron.Astrophys. 652, C4 (2021)]
2020 arXiv
-
[10]
BICEP2 / Keck Array x: Constraints on Primordial Gravitational Waves using Planck, WMAP, and New BICEP2/Keck Observations through the 2015 Season,
BICEP2, Keck Array Collaboration, P. A. R. Ade et al., “BICEP2 / Keck Array x: Constraints on Primordial Gravitational Waves using Planck, WMAP, and New BICEP2/Keck Observations through the 2015 Season,” Phys. Rev. Lett. 121 (2018) 221301, arXiv:1810.05216 [astro-ph.CO]
2018 arXiv
-
[11]
Planck 2018 results. X. Constraints on inflation,
Planck Collaboration, Y. Akrami et al., “Planck 2018 results. X. Constraints on inflation,” Astron. Astrophys. 641 (2020) A10, arXiv:1807.06211 [astro-ph.CO]
2020 arXiv
-
[12]
Improved Constraints on Primordial Gravitational Waves using Planck, WMAP, and BICEP/Keck Observations through the 2018 Observing Season,
BICEP, Keck Collaboration, P. A. R. Ade et al., “Improved Constraints on Primordial Gravitational Waves using Planck, WMAP, and BICEP/Keck Observations through the 2018 Observing Season,” Phys. Rev. Lett. 127 (2021) no. 15, 151301, arXiv:2110.00483 16 [astro-ph.CO]
2021
-
[13]
The First Three Seconds: a Review of Possible Expansion Histories of the Early Universe,
R. Allahverdi et al., “The First Three Seconds: a Review of Possible Expansion Histories of the Early Universe,” arXiv:2006.16182 [astro-ph.CO]
2006 arXiv
-
[14]
Deflationary universe scenario,
B. Spokoiny, “Deflationary universe scenario,” Phys. Lett. B 315 (1993) 40–45, arXiv:gr-qc/9306008
1993 arXiv
-
[15]
Electroweak Baryogenesis and the Expansion Rate of the Universe,
M. Joyce, “Electroweak Baryogenesis and the Expansion Rate of the Universe,” Phys. Rev. D 55 (1997) 1875–1878, arXiv:hep-ph/9606223
1997 arXiv
-
[16]
Cosmology with a primordial scaling field,
P. G. Ferreira and M. Joyce, “Cosmology with a primordial scaling field,” Phys. Rev. D 58 (1998) 023503, arXiv:astro-ph/9711102
1998 arXiv
-
[17]
Primordial Gravitational Wave Signals in Modified Cosmologies,
N. Bernal, A. Ghoshal, F. Hajkarim, and G. Lambiase, “Primordial Gravitational Wave Signals in Modified Cosmologies,” JCAP 11 (2020) 051, arXiv:2008.04959 [gr-qc]
2020 arXiv
-
[18]
Enhanced primordial gravitational waves from a stiff postinflationary era due to an oscillating inflaton,
C. Chen, K. Dimopoulos, C. Er¨ oncel, and A. Ghoshal, “Enhanced primordial gravitational waves from a stiff postinflationary era due to an oscillating inflaton,” Phys. Rev. D 110 (2024) no. 6, 063554, arXiv:2405.01679 [hep-ph]
2024 arXiv
-
[19]
Accounting for the time evolution of the equation of state parameter during reheating,
P. Saha, S. Anand, and L. Sriramkumar, “Accounting for the time evolution of the equation of state parameter during reheating,” Phys. Rev. D 102 (2020) no. 10, 103511, arXiv:2005.01874 [astro-ph.CO]
2020 arXiv
-
[20]
Signatures of non-thermal dark matter with kination and early matter domination. Gravitational waves versus laboratory searches,
A. Ghoshal, L. Heurtier, and A. Paul, “Signatures of non-thermal dark matter with kination and early matter domination. Gravitational waves versus laboratory searches,” JHEP 12 (2022) 105, arXiv:2208.01670 [hep-ph]
2022 arXiv
-
[21]
Cosmological Backgrounds of Gravitational Waves,
C. Caprini and D. G. Figueroa, “Cosmological Backgrounds of Gravitational Waves,” Class. Quant. Grav. 35 (2018) no. 16, 163001, arXiv:1801.04268 [astro-ph.CO]
2018 arXiv
-
[22]
Gravitational waves constraints on postinflationary phases stiffer than radiation,
M. Giovannini, “Gravitational waves constraints on postinflationary phases stiffer than radiation,” Phys. Rev. D 58 (1998) 083504, arXiv:hep-ph/9806329
1998 arXiv
-
[23]
Stochastic backgrounds of relic gravitons: a theoretical appraisal,
M. Giovannini, “Stochastic backgrounds of relic gravitons: a theoretical appraisal,” PMC Phys. A 4 (2010) 1, arXiv:0901.3026 [astro-ph.CO]
2010 arXiv
-
[24]
Quintessence and gravitational waves,
A. Riazuelo and J.-P. Uzan, “Quintessence and gravitational waves,” Phys. Rev. D 62 (2000) 083506, arXiv:astro-ph/0004156
2000 arXiv
-
[25]
Relic gravity waves from brane world inflation,
V. Sahni, M. Sami, and T. Souradeep, “Relic gravity waves from brane world inflation,” Phys. Rev. D 65 (2002) 023518, arXiv:gr-qc/0105121. 17
2002 arXiv
-
[26]
Probing the equation of state of the early universe with a space laser interferometer,
N. Seto and J. Yokoyama, “Probing the equation of state of the early universe with a space laser interferometer,” J. Phys. Soc. Jap. 72 (2003) 3082–3086, arXiv:gr-qc/0305096
2003 arXiv
-
[27]
Reheating after quintessential inflation and gravitational waves,
H. Tashiro, T. Chiba, and M. Sasaki, “Reheating after quintessential inflation and gravitational waves,” Class. Quant. Grav. 21 (2004) 1761–1772, arXiv:gr-qc/0307068
2004 arXiv
-
[28]
Space laser interferometers can determine the thermal history of the early Universe,
K. Nakayama, S. Saito, Y. Suwa, and J. Yokoyama, “Space laser interferometers can determine the thermal history of the early Universe,” Phys. Rev. D 77 (2008) 124001, arXiv:0802.2452 [hep-ph]
2008 arXiv
-
[29]
Probing reheating temperature of the universe with gravitational wave background,
K. Nakayama, S. Saito, Y. Suwa, and J. Yokoyama, “Probing reheating temperature of the universe with gravitational wave background,” JCAP 06 (2008) 020, arXiv:0804.1827 [astro-ph]
2008 arXiv
-
[30]
Testing Superstring Theories with Gravitational Waves,
R. Durrer and J. Hasenkamp, “Testing Superstring Theories with Gravitational Waves,” Phys. Rev. D 84 (2011) 064027, arXiv:1105.5283 [gr-qc]
2011 arXiv
-
[31]
Prospects for determination of thermal history after inflation with future gravitational wave detectors,
S. Kuroyanagi, K. Nakayama, and S. Saito, “Prospects for determination of thermal history after inflation with future gravitational wave detectors,” Phys. Rev. D 84 (2011) 123513, arXiv:1110.4169 [astro-ph.CO]
2011 arXiv
-
[32]
Probing the Universe through the Stochastic Gravitational Wave Background,
S. Kuroyanagi, T. Chiba, and T. Takahashi, “Probing the Universe through the Stochastic Gravitational Wave Background,” JCAP 11 (2018) 038, arXiv:1807.00786 [astro-ph.CO]
2018 arXiv
-
[33]
Decoding the phases of early and late time reheating through imprints on primordial gravitational waves,
M. R. Haque, D. Maity, T. Paul, and L. Sriramkumar, “Decoding the phases of early and late time reheating through imprints on primordial gravitational waves,” Phys. Rev. D 104 (2021) no. 6, 063513, arXiv:2105.09242 [astro-ph.CO]
2021 arXiv
-
[34]
Probing dark radiation with inflationary gravitational waves,
R. Jinno, T. Moroi, and K. Nakayama, “Probing dark radiation with inflationary gravitational waves,” Phys. Rev. D 86 (2012) 123502, arXiv:1208.0184 [astro-ph.CO]
2012 arXiv
-
[35]
Gravitational-wave cosmology across 29 decades in frequency,
P. D. Lasky et al., “Gravitational-wave cosmology across 29 decades in frequency,” Phys. Rev. X 6 (2016) no. 1, 011035, arXiv:1511.05994 [astro-ph.CO]
2016 arXiv
-
[36]
Bose-Einstein-condensed scalar field dark matter and the gravitational wave background from inflation: new cosmological constraints and its detectability by LIGO,
B. Li, P. R. Shapiro, and T. Rindler-Daller, “Bose-Einstein-condensed scalar field dark matter and the gravitational wave background from inflation: new cosmological constraints and its detectability by LIGO,” Phys. Rev. D 96 (2017) no. 6, 063505, arXiv:1611.07961 [astro-ph.CO]
2017 arXiv
-
[37]
Primordial gravitational waves, precisely: The role of thermodynamics in the Standard Model,
K. Saikawa and S. Shirai, “Primordial gravitational waves, precisely: The role of thermodynamics in the Standard Model,” JCAP 05 (2018) 035, arXiv:1803.01038 18 [hep-ph]
2018 arXiv
-
[38]
Using a Primordial Gravitational Wave Background to Illuminate New Physics,
R. R. Caldwell, T. L. Smith, and D. G. E. Walker, “Using a Primordial Gravitational Wave Background to Illuminate New Physics,” Phys. Rev. D 100 (2019) no. 4, 043513, arXiv:1812.07577 [astro-ph.CO]
2019 arXiv
-
[39]
Primordial Gravitational Waves in Nonstandard Cosmologies,
N. Bernal and F. Hajkarim, “Primordial Gravitational Waves in Nonstandard Cosmologies,” Phys. Rev. D 100 (2019) no. 6, 063502, arXiv:1905.10410 [astro-ph.CO]
2019 arXiv
-
[40]
Ability of LIGO and LISA to probe the equation of state of the early Universe,
D. G. Figueroa and E. H. Tanin, “Ability of LIGO and LISA to probe the equation of state of the early Universe,” JCAP 08 (2019) 011, arXiv:1905.11960 [astro-ph.CO]
2019 arXiv
-
[41]
Imprint of a scalar era on the primordial spectrum of gravitational waves,
F. D’Eramo and K. Schmitz, “Imprint of a scalar era on the primordial spectrum of gravitational waves,” Phys. Rev. Research. 1 (2019) 013010, arXiv:1904.07870 [hep-ph]
2019 arXiv
-
[42]
Cosmological Constraints on Bose-Einstein-Condensed Scalar Field Dark Matter,
B. Li, T. Rindler-Daller, and P. R. Shapiro, “Cosmological Constraints on Bose-Einstein-Condensed Scalar Field Dark Matter,” Phys. Rev. D 89 (2014) no. 8, 083536, arXiv:1310.6061 [astro-ph.CO]
2014 arXiv
-
[43]
Quantitative predictions for f(R) gravity primordial gravitational waves,
S. D. Odintsov, V. K. Oikonomou, and F. P. Fronimos, “Quantitative predictions for f(R) gravity primordial gravitational waves,” Phys. Dark Univ. 35 (2022) 100950, arXiv:2108.11231 [gr-qc]
2022 arXiv
-
[44]
Pre-inflationary bounce effects on primordial gravitational waves of f(R) gravity,
S. D. Odintsov and V. K. Oikonomou, “Pre-inflationary bounce effects on primordial gravitational waves of f(R) gravity,” Phys. Lett. B 824 (2022) 136817, arXiv:2112.02584 [gr-qc]
2022 arXiv
-
[45]
Precision cosmology and the stiff-amplified gravitational-wave background from inflation: NANOGrav, Advanced LIGO-Virgo and the Hubble tension,
B. Li and P. R. Shapiro, “Precision cosmology and the stiff-amplified gravitational-wave background from inflation: NANOGrav, Advanced LIGO-Virgo and the Hubble tension,” JCAP 10 (2021) 024, arXiv:2107.12229 [astro-ph.CO]
2021 arXiv
-
[46]
Waterfall stiff period can generate observable primordial gravitational waves,
K. Dimopoulos, “Waterfall stiff period can generate observable primordial gravitational waves,” JCAP 10 (2022) 027, arXiv:2206.02264 [hep-ph]
2022 arXiv
-
[47]
Gravitational wave and CMB probes of axion kination,
R. T. Co, D. Dunsky, N. Fernandez, A. Ghalsasi, L. J. Hall, K. Harigaya, and J. Shelton, “Gravitational wave and CMB probes of axion kination,” JHEP 09 (2022) 116, arXiv:2108.09299 [hep-ph]
2022 arXiv
-
[48]
Implications of the NANOGrav results for inflation,
S. Vagnozzi, “Implications of the NANOGrav results for inflation,” Mon. Not. Roy. Astron. Soc. 502 (2021) no. 1, L11–L15, arXiv:2009.13432 [astro-ph.CO]
2021 arXiv
-
[49]
Primordial gravitational waves from NANOGrav: A broken power-law approach,
M. Benetti, L. L. Graef, and S. Vagnozzi, “Primordial gravitational waves from NANOGrav: A broken power-law approach,” Phys. Rev. D 105 (2022) no. 4, 043520, 19 arXiv:2111.04758 [astro-ph.CO]
2022 arXiv
-
[50]
Causal gravitational waves as a probe of free streaming particles and the expansion of the Universe,
A. Hook, G. Marques-Tavares, and D. Racco, “Causal gravitational waves as a probe of free streaming particles and the expansion of the Universe,” JHEP 02 (2021) 117, arXiv:2010.03568 [hep-ph]
2021 arXiv
-
[51]
Kination cosmology from scalar fields and gravitational-wave signatures,
Y. Gouttenoire, G. Servant, and P. Simakachorn, “Kination cosmology from scalar fields and gravitational-wave signatures,” arXiv:2111.01150 [hep-ph]
-
[52]
Review of Particle Physics,
Particle Data Group Collaboration, P. A. Zyla et al., “Review of Particle Physics,” PTEP 2020 (2020) no. 8, 083C01
2020
-
[53]
µ→eγ at a Rate of One Out of 10 9 Muon Decays?,
P. Minkowski, “µ→eγ at a Rate of One Out of 10 9 Muon Decays?,” Phys. Lett. B 67 (1977) 421–428
1977
-
[54]
Horizontal gauge symmetry and masses of neutrinos,
T. Yanagida, “Horizontal gauge symmetry and masses of neutrinos,” Conf. Proc. C 7902131 (1979) 95–99
1979
-
[55]
Complex Spinors and Unified Theories,
M. Gell-Mann, P. Ramond, and R. Slansky, “Complex Spinors and Unified Theories,” Conf. Proc. C 790927 (1979) 315–321, arXiv:1306.4669 [hep-th]
1979 arXiv
-
[56]
Neutrino Mass and Spontaneous Parity Nonconservation,
R. N. Mohapatra and G. Senjanovic, “Neutrino Mass and Spontaneous Parity Nonconservation,” Phys. Rev. Lett. 44 (1980) 912
1980
-
[57]
Neutrino Masses in SU(2) x U(1) Theories,
J. Schechter and J. W. F. Valle, “Neutrino Masses in SU(2) x U(1) Theories,” Phys. Rev. D 22 (1980) 2227
1980
-
[58]
U(1) as the Minimal Horizontal Gauge Symmetry,
A. Davidson, M. Koca, and K. C. Wali, “U(1) as the Minimal Horizontal Gauge Symmetry,” Phys. Rev. Lett. 43 (1979) 92
1979
-
[59]
Local B-L Symmetry of Electroweak Interactions, Majorana Neutrinos and Neutron Oscillations,
R. N. Mohapatra and R. E. Marshak, “Local B-L Symmetry of Electroweak Interactions, Majorana Neutrinos and Neutron Oscillations,” Phys. Rev. Lett. 44 (1980) 1316–1319. [Erratum: Phys.Rev.Lett. 44, 1643 (1980)]
1980
-
[60]
Quark - Lepton Symmetry and B-L as the U(1) Generator of the Electroweak Symmetry Group,
R. E. Marshak and R. N. Mohapatra, “Quark - Lepton Symmetry and B-L as the U(1) Generator of the Electroweak Symmetry Group,” Phys. Lett. B 91 (1980) 222–224
1980
-
[61]
B−L as the fourth color within an SU(2) L× U(1)R× U(1) model,
A. Davidson, “ B−L as the fourth color within an SU(2) L× U(1)R× U(1) model,” Phys. Rev. D 20 (1979) 776
1979
-
[62]
Universal Seesaw Mechanism?,
A. Davidson and K. C. Wali, “Universal Seesaw Mechanism?,” Phys. Rev. Lett. 59 (1987) 393
1987
-
[63]
Neutrino Masses and the Scale of B-L Violation,
C. Wetterich, “Neutrino Masses and the Scale of B-L Violation,” Nucl. Phys. B 187 (1981) 343–375. 20
1981
-
[64]
B−l Violating Proton Decay and Late Cosmological Baryon Production,
A. Masiero, J. F. Nieves, and T. Yanagida, “ B−l Violating Proton Decay and Late Cosmological Baryon Production,” Phys. Lett. B 116 (1982) 11–15
1982
-
[65]
Spontaneous Breaking of Global B−l Symmetry and Matter - Antimatter Oscillations in Grand Unified Theories,
R. N. Mohapatra and G. Senjanovic, “Spontaneous Breaking of Global B−l Symmetry and Matter - Antimatter Oscillations in Grand Unified Theories,” Phys. Rev. D 27 (1983) 254
1983
-
[66]
Neutrino masses, neutral vector bosons and the scale of B-L breaking,
W. Buchmuller, C. Greub, and P. Minkowski, “Neutrino masses, neutral vector bosons and the scale of B-L breaking,” Phys. Lett. B 267 (1991) 395–399
1991
-
[67]
Nonexotic Neutral Gauge Bosons,
T. Appelquist, B. A. Dobrescu, and A. R. Hopper, “Nonexotic Neutral Gauge Bosons,” Phys. Rev. D 68 (2003) 035012, arXiv:hep-ph/0212073
2003 arXiv
-
[68]
Classically conformal U(1)’ extended standard model and Higgs vacuum stability,
S. Oda, N. Okada, and D.-s. Takahashi, “Classically conformal U(1)’ extended standard model and Higgs vacuum stability,” Phys. Rev. D 92 (2015) no. 1, 015026, arXiv:1504.06291 [hep-ph]
2015 arXiv
-
[69]
Electroweak vacuum stability in classically conformal B-L extension of the Standard Model,
A. Das, N. Okada, and N. Papapietro, “Electroweak vacuum stability in classically conformal B-L extension of the Standard Model,” Eur. Phys. J. C 77 (2017) no. 2, 122, arXiv:1509.01466 [hep-ph]
2017 arXiv
-
[70]
Classically conformal U(1)’ extended standard model, electroweak vacuum stability, and LHC Run-2 bounds,
A. Das, S. Oda, N. Okada, and D.-s. Takahashi, “Classically conformal U(1)’ extended standard model, electroweak vacuum stability, and LHC Run-2 bounds,” Phys. Rev. D 93 (2016) no. 11, 115038, arXiv:1605.01157 [hep-ph]
2016 arXiv
-
[71]
Cold Dark Matter from heavy Right-Handed neutrino mixing,
A. Anisimov and P. Di Bari, “Cold Dark Matter from heavy Right-Handed neutrino mixing,” Phys. Rev. D 80 (2009) 073017, arXiv:0812.5085 [hep-ph]
2009 arXiv
-
[72]
Higgs portal dark matter in the minimal gauged U(1)B−L model,
N. Okada and O. Seto, “Higgs portal dark matter in the minimal gauged U(1)B−L model,” Phys. Rev. D 82 (2010) 023507, arXiv:1002.2525 [hep-ph]
2010 arXiv
-
[73]
Z′ BL portal dark matter and LHC Run-2 results,
N. Okada and S. Okada, “ Z′ BL portal dark matter and LHC Run-2 results,” Phys. Rev. D 93 (2016) no. 7, 075003, arXiv:1601.07526 [hep-ph]
2016 arXiv
-
[74]
Z′-portal right-handed neutrino dark matter in the minimal U(1)X extended Standard Model,
N. Okada and S. Okada, “ Z′-portal right-handed neutrino dark matter in the minimal U(1)X extended Standard Model,” Phys. Rev. D 95 (2017) no. 3, 035025, arXiv:1611.02672 [hep-ph]
2017 arXiv
-
[75]
Enhanced pair production of heavy Majorana neutrinos at the LHC,
A. Das, N. Okada, and D. Raut, “Enhanced pair production of heavy Majorana neutrinos at the LHC,” Phys. Rev. D 97 (2018) no. 11, 115023, arXiv:1710.03377 [hep-ph]
2018 arXiv
-
[76]
Heavy Majorana neutrino pair productions at the LHC in minimal U(1) extended Standard Model,
A. Das, N. Okada, and D. Raut, “Heavy Majorana neutrino pair productions at the LHC in minimal U(1) extended Standard Model,” Eur. Phys. J. C 78 (2018) no. 9, 696, arXiv:1711.09896 [hep-ph] . 21
2018 arXiv
-
[77]
Probing the seesaw mechanism at the 250 GeV ILC,
A. Das, N. Okada, S. Okada, and D. Raut, “Probing the seesaw mechanism at the 250 GeV ILC,” Phys. Lett. B 797 (2019) 134849, arXiv:1812.11931 [hep-ph]
2019 arXiv
-
[78]
Non-Minimal B-L Inflation with Observable Gravity Waves,
N. Okada, M. U. Rehman, and Q. Shafi, “Non-Minimal B-L Inflation with Observable Gravity Waves,” Phys. Lett. B 701 (2011) 520–525, arXiv:1102.4747 [hep-ph]
2011 arXiv
-
[79]
Inflection-point Higgs Inflation,
N. Okada and D. Raut, “Inflection-point Higgs Inflation,” Phys. Rev. D 95 (2017) no. 3, 035035, arXiv:1610.09362 [hep-ph]
2017 arXiv
-
[80]
Double Inflation in Classically Conformal B−L Model,
A. Ghoshal, N. Okada, A. Paul, and D. Raut, “Double Inflation in Classically Conformal B−L Model,” arXiv:2405.10537 [astro-ph.CO]
-
[81]
Gauge Coupling Renormalization With Several U(1) Factors,
F. del Aguila, G. D. Coughlan, and M. Quiros, “Gauge Coupling Renormalization With Several U(1) Factors,” Nucl. Phys. B 307 (1988) 633. [Erratum: Nucl.Phys.B 312, 751 (1989)]
1988
-
[82]
SU(5) ×U(1)X grand unification with minimal seesaw and Z′-portal dark matter,
N. Okada, S. Okada, and D. Raut, “SU(5) ×U(1)X grand unification with minimal seesaw and Z′-portal dark matter,” Phys. Lett. B 780 (2018) 422–426, arXiv:1712.05290 [hep-ph]
2018 arXiv
-
[83]
Baryogenesis Without Grand Unification,
M. Fukugita and T. Yanagida, “Baryogenesis Without Grand Unification,” Phys. Lett. B 174 (1986) 45–47
1986
-
[84]
The Observational Status of Simple Inflationary Models: an Update,
N. Okada, V. N. S ¸eno˘ guz, and Q. Shafi, “The Observational Status of Simple Inflationary Models: an Update,” Turk. J. Phys. 40 (2016) no. 2, 150–162, arXiv:1403.6403 [hep-ph]
2016 arXiv
-
[85]
Cosmological perturbations in coherent oscillating scalar field models,
J. A. R. Cembranos, A. L. Maroto, and S. J. N´ u˜ nez Jare˜ no, “Cosmological perturbations in coherent oscillating scalar field models,” JHEP 03 (2016) 013, arXiv:1509.08819 [astro-ph.CO]
2016 arXiv
-
[86]
Radiative Corrections as the Origin of Spontaneous Symmetry Breaking,
S. R. Coleman and E. J. Weinberg, “Radiative Corrections as the Origin of Spontaneous Symmetry Breaking,” Phys. Rev. D 7 (1973) 1888–1910
1973
-
[87]
Revisiting the ultraviolet tail of the primordial gravitational wave,
S. Pi, M. Sasaki, A. Wang, and J. Wang, “Revisiting the ultraviolet tail of the primordial gravitational wave,” Phys. Rev. D 110 (2024) no. 10, 103529, arXiv:2407.06066 [astro-ph.CO]
2024 arXiv
-
[88]
Laser Interferometer Space Antenna,
LISA Collaboration, P. Amaro-Seoane et al., “Laser Interferometer Space Antenna,” arXiv:1702.00786 [astro-ph.IM]
-
[89]
The Laser Interferometer Space Antenna: Unveiling the Millihertz Gravitational Wave Sky,
J. Baker et al., “The Laser Interferometer Space Antenna: Unveiling the Millihertz Gravitational Wave Sky,” arXiv:1907.06482 [astro-ph.IM] . 22
1907 arXiv
-
[90]
Beyond LISA: Exploring future gravitational wave missions,
J. Crowder and N. J. Cornish, “Beyond LISA: Exploring future gravitational wave missions,” Phys. Rev. D 72 (2005) 083005, arXiv:gr-qc/0506015
2005 arXiv
-
[91]
Detecting the cosmic gravitational wave background with the big bang observer,
V. Corbin and N. J. Cornish, “Detecting the cosmic gravitational wave background with the big bang observer,” Class. Quant. Grav. 23 (2006) 2435–2446, arXiv:gr-qc/0512039
2006 arXiv
-
[92]
Laser interferometry for the big bang observer,
G. M. Harry, P. Fritschel, D. A. Shaddock, W. Folkner, and E. S. Phinney, “Laser interferometry for the big bang observer,” Class. Quant. Grav. 23 (2006) 4887–4894. [Erratum: Class.Quant.Grav. 23, 7361 (2006)]
2006
-
[93]
Possibility of direct measurement of the acceleration of the universe using 0.1-Hz band laser interferometer gravitational wave antenna in space,
N. Seto, S. Kawamura, and T. Nakamura, “Possibility of direct measurement of the acceleration of the universe using 0.1-Hz band laser interferometer gravitational wave antenna in space,” Phys. Rev. Lett. 87 (2001) 221103, arXiv:astro-ph/0108011
2001 arXiv
-
[94]
The Japanese space gravitational wave antenna DECIGO,
S. Kawamura et al., “The Japanese space gravitational wave antenna DECIGO,” Class. Quant. Grav. 23 (2006) S125–S132
2006
-
[95]
Detector configuration of DECIGO/BBO and identification of cosmological neutron-star binaries,
K. Yagi and N. Seto, “Detector configuration of DECIGO/BBO and identification of cosmological neutron-star binaries,” Phys. Rev. D 83 (2011) 044011, arXiv:1101.3940 [astro-ph.CO]. [Erratum: Phys.Rev.D 95, 109901 (2017)]
2011 arXiv
-
[96]
Exploring the Sensitivity of Next Generation Gravitational Wave Detectors,
LIGO Scientific Collaboration, B. P. Abbott et al., “Exploring the Sensitivity of Next Generation Gravitational Wave Detectors,” Class. Quant. Grav. 34 (2017) no. 4, 044001, arXiv:1607.08697 [astro-ph.IM]
2017 arXiv
-
[97]
Cosmic Explorer: The U.S. Contribution to Gravitational-Wave Astronomy beyond LIGO,
D. Reitze et al., “Cosmic Explorer: The U.S. Contribution to Gravitational-Wave Astronomy beyond LIGO,” Bull. Am. Astron. Soc. 51 (2019) no. 7, 035, arXiv:1907.04833 [astro-ph.IM]
2019 arXiv
-
[98]
The Einstein Telescope: A third-generation gravitational wave observatory,
M. Punturo et al., “The Einstein Telescope: A third-generation gravitational wave observatory,” Class. Quant. Grav. 27 (2010) 194002
2010
-
[99]
Sensitivity Studies for Third-Generation Gravitational Wave Observatories,
S. Hild et al., “Sensitivity Studies for Third-Generation Gravitational Wave Observatories,” Class. Quant. Grav. 28 (2011) 094013, arXiv:1012.0908 [gr-qc]
2011 arXiv
-
[100]
Scientific Objectives of Einstein Telescope,
B. Sathyaprakash et al., “Scientific Objectives of Einstein Telescope,” Class. Quant. Grav. 29 (2012) 124013, arXiv:1206.0331 [gr-qc] . [Erratum: Class.Quant.Grav. 30, 079501 (2013)]
2012 arXiv
-
[101]
Science Case for the Einstein Telescope,
ET Collaboration, M. Maggiore et al., “Science Case for the Einstein Telescope,” JCAP 03 (2020) 050, arXiv:1912.02622 [astro-ph.CO] . 23
2020 arXiv
-
[102]
Unveiling the gravitational universe at µ-Hz frequencies,
A. Sesana et al., “Unveiling the gravitational universe at µ-Hz frequencies,” Exper. Astron. 51 (2021) no. 3, 1333–1383, arXiv:1908.11391 [astro-ph.IM]
2021 arXiv
-
[103]
Advanced LIGO: The next generation of gravitational wave detectors,
LIGO Scientific Collaboration, G. M. Harry, “Advanced LIGO: The next generation of gravitational wave detectors,” Class. Quant. Grav. 27 (2010) 084006
2010
-
[104]
Advanced LIGO,
LIGO Scientific Collaboration, J. Aasi et al., “Advanced LIGO,” Class. Quant. Grav. 32 (2015) 074001, arXiv:1411.4547 [gr-qc]
2015 arXiv
-
[105]
Advanced Virgo: a second-generation interferometric gravitational wave detector,
VIRGO Collaboration, F. Acernese et al., “Advanced Virgo: a second-generation interferometric gravitational wave detector,” Class. Quant. Grav. 32 (2015) no. 2, 024001, arXiv:1408.3978 [gr-qc]
2015 arXiv
-
[106]
Open data from the first and second observing runs of Advanced LIGO and Advanced Virgo,
LIGO Scientific, Virgo Collaboration, R. Abbott et al., “Open data from the first and second observing runs of Advanced LIGO and Advanced Virgo,” SoftwareX 13 (2021) 100658, arXiv:1912.11716 [gr-qc]
2021 arXiv
-
[107]
Doubling of Weak Gauge Bosons in an Extension of the Standard Model,
V. D. Barger, W.-Y. Keung, and E. Ma, “Doubling of Weak Gauge Bosons in an Extension of the Standard Model,” Phys. Rev. Lett. 44 (1980) 1169
1980
-
[108]
Search for high-mass dilepton resonances using 139 fb−1 of pp collision data collected at√s =13 TeV with the ATLAS detector,
ATLAS Collaboration, G. Aad et al., “Search for high-mass dilepton resonances using 139 fb−1 of pp collision data collected at√s =13 TeV with the ATLAS detector,” Phys. Lett. B 796 (2019) 68–87, arXiv:1903.06248 [hep-ex]
2019 arXiv
-
[109]
Search for a narrow resonance in high-mass dilepton final states in proton-proton collisions using 140 fb−1 of data at√s = 13 TeV,
CMS Collaboration, “Search for a narrow resonance in high-mass dilepton final states in proton-proton collisions using 140 fb−1 of data at√s = 13 TeV,”
-
[110]
New generation of parton distributions with uncertainties from global QCD analysis,
J. Pumplin, D. R. Stump, J. Huston, H. L. Lai, P. M. Nadolsky, and W. K. Tung, “New generation of parton distributions with uncertainties from global QCD analysis,” JHEP 07 (2002) 012, arXiv:hep-ph/0201195
2002 arXiv
-
[111]
Challenges and opportunities of gravitational-wave searches at MHz to GHz frequencies,
N. Aggarwal et al., “Challenges and opportunities of gravitational-wave searches at MHz to GHz frequencies,” Living Rev. Rel. 24 (2021) no. 1, 4, arXiv:2011.12414 [gr-qc]
2021 arXiv
-
[112]
Microwave apparatus for gravitational waves observation,
R. Ballantini et al., “Microwave apparatus for gravitational waves observation,” arXiv:gr-qc/0502054
-
[113]
Detecting high-frequency gravitational waves with optically-levitated sensors,
A. Arvanitaki and A. A. Geraci, “Detecting high-frequency gravitational waves with optically-levitated sensors,” Phys. Rev. Lett. 110 (2013) no. 7, 071105, arXiv:1207.5320 [gr-qc]
2013 arXiv
-
[114]
Upper limits on the amplitude of ultra-high-frequency gravitational waves from graviton to photon conversion,
A. Ejlli, D. Ejlli, A. M. Cruise, G. Pisano, and H. Grote, “Upper limits on the amplitude of ultra-high-frequency gravitational waves from graviton to photon conversion,” Eur. Phys. J. 24 C 79 (2019) no. 12, 1032, arXiv:1908.00232 [gr-qc]
2019 arXiv
-
[115]
Searching for New Physics with a Levitated-Sensor-Based Gravitational-Wave Detector,
N. Aggarwal, G. P. Winstone, M. Teo, M. Baryakhtar, S. L. Larson, V. Kalogera, and A. A. Geraci, “Searching for New Physics with a Levitated-Sensor-Based Gravitational-Wave Detector,” Phys. Rev. Lett. 128 (2022) no. 11, 111101, arXiv:2010.13157 [gr-qc]
2022 arXiv
-
[116]
Optical Trapping of High-Aspect-Ratio NaYF Hexagonal Prisms for kHz-MHz Gravitational Wave Detectors,
LSD Collaboration, G. Winstone et al., “Optical Trapping of High-Aspect-Ratio NaYF Hexagonal Prisms for kHz-MHz Gravitational Wave Detectors,” Phys. Rev. Lett. 129 (2022) no. 5, 053604, arXiv:2204.10843 [physics.optics]
2022 arXiv
-
[117]
Detecting high-frequency gravitational waves with microwave cavities,
A. Berlin, D. Blas, R. Tito D’Agnolo, S. A. R. Ellis, R. Harnik, Y. Kahn, and J. Sch¨ utte-Engel, “Detecting high-frequency gravitational waves with microwave cavities,” Phys. Rev. D 105 (2022) no. 11, 116011, arXiv:2112.11465 [hep-ph]
2022 arXiv
-
[118]
Searches for New Particles, Dark Matter, and Gravitational Waves with SRF Cavities,
A. Berlin et al., “Searches for New Particles, Dark Matter, and Gravitational Waves with SRF Cavities,” arXiv:2203.12714 [hep-ph]
-
[119]
Electromagnetic cavities as mechanical bars for gravitational waves,
A. Berlin, D. Blas, R. Tito D’Agnolo, S. A. R. Ellis, R. Harnik, Y. Kahn, J. Sch¨ utte-Engel, and M. Wentzel, “Electromagnetic cavities as mechanical bars for gravitational waves,” Phys. Rev. D 108 (2023) no. 8, 084058, arXiv:2303.01518 [hep-ph]
2023 arXiv
-
[120]
Rare Events Detected with a Bulk Acoustic Wave High Frequency Gravitational Wave Antenna,
M. Goryachev, W. M. Campbell, I. S. Heng, S. Galliou, E. N. Ivanov, and M. E. Tobar, “Rare Events Detected with a Bulk Acoustic Wave High Frequency Gravitational Wave Antenna,” Phys. Rev. Lett. 127 (2021) no. 7, 071102, arXiv:2102.05859 [gr-qc]
2021 arXiv
-
[121]
Gravitational Wave Detection with High Frequency Phonon Trapping Acoustic Cavities,
M. Goryachev and M. E. Tobar, “Gravitational Wave Detection with High Frequency Phonon Trapping Acoustic Cavities,” Phys. Rev. D 90 (2014) no. 10, 102005, arXiv:1410.2334 [gr-qc] . [Erratum: Phys.Rev.D 108, 129901 (2023)]
2014 arXiv
-
[122]
Author Correction: The multi-mode acoustic gravitational wave experiment: MAGE [doi: 10.1038/s41598-023-35670-y],
W. M. Campbell, M. Goryachev, and M. E. Tobar, “Author Correction: The multi-mode acoustic gravitational wave experiment: MAGE [doi: 10.1038/s41598-023-35670-y],” Sci. Rep. 13 (2023) no. 1, 10638, arXiv:2307.00715 [gr-qc]
2023 arXiv
-
[123]
High-Frequency Gravitational Waves in Electromagnetic Waveguides,
F. Sorge, “High-Frequency Gravitational Waves in Electromagnetic Waveguides,” Annalen Phys. 535 (2023) no. 10, 2300228
2023
-
[124]
Detecting single gravitons with quantum sensing,
G. Tobar, S. K. Manikandan, T. Beitel, and I. Pikovski, “Detecting single gravitons with quantum sensing,” Nature Commun. 15 (2024) no. 1, 7229, arXiv:2308.15440 [quant-ph]
2024 arXiv
-
[125]
Graviton detection and the quantization of gravity,
D. Carney, V. Domcke, and N. L. Rodd, “Graviton detection and the quantization of gravity,” Phys. Rev. D 109 (2024) no. 4, 044009, arXiv:2308.12988 [hep-th] . 25
2024 arXiv
-
[126]
Novel Search for High-Frequency Gravitational Waves with Low-Mass Axion Haloscopes,
V. Domcke, C. Garcia-Cely, and N. L. Rodd, “Novel Search for High-Frequency Gravitational Waves with Low-Mass Axion Haloscopes,” Phys. Rev. Lett. 129 (2022) no. 4, 041101, arXiv:2202.00695 [hep-ph]
2022 arXiv
-
[127]
Symmetries and selection rules: optimising axion haloscopes for Gravitational Wave searches,
V. Domcke, C. Garcia-Cely, S. M. Lee, and N. L. Rodd, “Symmetries and selection rules: optimising axion haloscopes for Gravitational Wave searches,” JHEP 03 (2024) 128, arXiv:2306.03125 [hep-ph]
2024 arXiv
-
[128]
High-frequency gravitational wave detection via optical frequency modulation,
T. Bringmann, V. Domcke, E. Fuchs, and J. Kopp, “High-frequency gravitational wave detection via optical frequency modulation,” Phys. Rev. D 108 (2023) no. 6, L061303, arXiv:2304.10579 [hep-ph]
2023 arXiv
-
[129]
Detection of high-frequency gravitational waves using high-energy pulsed lasers,
G. Vacalis, G. Marocco, J. Bamber, R. Bingham, and G. Gregori, “Detection of high-frequency gravitational waves using high-energy pulsed lasers,” Class. Quant. Grav. 40 (2023) no. 15, 155006, arXiv:2301.08163 [gr-qc]
2023 arXiv
-
[130]
Limits on High-Frequency Gravitational Waves in Planetary Magnetospheres,
T. Liu, J. Ren, and C. Zhang, “Limits on High-Frequency Gravitational Waves in Planetary Magnetospheres,” Phys. Rev. Lett. 132 (2024) no. 13, 131402, arXiv:2305.01832 [hep-ph]
2024 arXiv
-
[131]
Probing GHz gravitational waves with graviton–magnon resonance,
A. Ito, T. Ikeda, K. Miuchi, and J. Soda, “Probing GHz gravitational waves with graviton–magnon resonance,” Eur. Phys. J. C 80 (2020) no. 3, 179, arXiv:1903.04843 [gr-qc]
2020 arXiv
-
[132]
A formalism for magnon gravitational wave detectors,
A. Ito and J. Soda, “A formalism for magnon gravitational wave detectors,” Eur. Phys. J. C 80 (2020) no. 6, 545, arXiv:2004.04646 [gr-qc]
2020 arXiv
-
[133]
Exploring high-frequency gravitational waves with magnons,
A. Ito and J. Soda, “Exploring high-frequency gravitational waves with magnons,” Eur. Phys. J. C 83 (2023) no. 8, 766, arXiv:2212.04094 [gr-qc]
2023 arXiv
-
[134]
Macroscopic quantum response to gravitational waves,
A. Ito and R. Kitano, “Macroscopic quantum response to gravitational waves,” JCAP 04 (2024) 068, arXiv:2309.02992 [gr-qc] . 26
2024 arXiv
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