Stability of fundamental couplings: A global analysis

Martins, C. J. A. P.; Pinho, Ana Marta

doi:10.1103/physrevd.95.023008

Cited by 34 publications

(34 citation statements)

References 66 publications

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“…and we shall consider three different numerical values, namely f = 0.09, 0.2, 0.9. We have chosen these values in agreement with the current dark matter constraints obtained from compact stars, main sequence stars and the Sun [56][57][58][59][60][61][62]. Actually, as shown by several authors, even smaller amounts of DM (as a percentage of the total mass of the star) can have a quite visible impact on the structure of stars [63][64][65].…”

Section: Hydrostatic Equilibriummentioning

confidence: 94%

Millisecond pulsars modeled as strange quark stars admixed with condensed dark matter

Panotopoulos

Lopes

2018

Int. J. Mod. Phys. D

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We study for the first time how a new class of stars could impact an ensemble of pulsars with known masses and spin-periods. These new compact objects are strange stars admixed with condensed dark matter. In this exploratory theoretical work, our goal is to determine how the basic parameters of pulsars are modified for such a new class of compact objects. In particular we consider three different scenarios that correspond to a dark matter mass fraction of 5%, 11% and 25%. Within each scenario with fixed parameters we predict theoretically other properties of the pulsars, such as the radius, the compactness, the moment of inertia, as well as the angular momentum. Our numerical results are summarized in tables and also shown graphically for better visualization, where a comparison between the different scenarios can be made.

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Section: Hydrostatic Equilibriummentioning

confidence: 94%

Millisecond pulsars modeled as strange quark stars admixed with condensed dark matter

Panotopoulos

Lopes

2018

Int. J. Mod. Phys. D

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“…On the observational side, claims have been made that the absorption spectra of distant quasars support cosmological time variation and a dipole in α [24][25][26][27][28]. More recent observations and analyses have failed to reproduce such a result consistently [29,30], calling into question the method (in particular, the spatial stability of the wavelength calibration) used to obtain the spatial dipole result [31]. Future efforts at the Very Large Telescope (VLT) [21] could improve sensitivity to α variations by an additional two orders of magnitude.…”

Section: Introductionmentioning

confidence: 99%

Probing spatial variation of the fine-structure constant using the CMB

et al. 2019

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The fine-structure constant, α, controls the strength of the electromagnetic interaction. There are extensions of the standard model in which α is dynamical on cosmological length and time-scales. The physics of the cosmic microwave background (CMB) depends on the value of α. The effects of spatial variation in α on the CMB are similar to those produced by weak lensing: smoothing of the power spectrum, and generation of non-Gaussian features. These would induce a bias to estimates of the weak-lensing potential power spectrum of the CMB. Using this effect, Planck measurements of the temperature and polarization power spectrum, as well as estimates of CMB lensing, are used to place limits (95% C. L.) on the amplitude of a scale-invariant angular power spectrum of α fluctuations relative to the mean value (C αThe limits depend on the assumed shape of the α-fluctuation power spectrum. For example, for a white noise angular power spectrum (C α L = A α WN ), the limit is A α WN ≤ 2.3 × 10 −8 . It is found that the response of the CMB to α fluctuations depends on a separate-universe approximation, such that theoretical predictions are only reliable for α multipoles with L 100 . An optimal trispectrum estimator can be constructed and it is found that it is only marginally more sensitive than lensing techniques for Planck but significantly more sensitive when considering the next generation of experiments. For a future CMB experiment with cosmic-variance limited polarization sensitivity (e.g., CMB-S4), the optimal estimator could detect α fluctuations with A α SI > 1.9 × 10 −6 and A α WN > 1.4 × 10 −9 .

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“…The presence of dark matter in the Sun's core could help solve the long-running solar composition problem [35], a discrepancy between the solar structure inferred from helioseismology and the one computed from a SSM by inputting the most up-to-date photospheric abundances [36,37]. This type of diagnostic has also been successfully extended to other stars, including other sun-like stars [e.g., 38,39] and neutron stars [40][41][42][43]. In addition, such types of studies have also been extended to the first generation of stars [44][45][46][47][48].…”

Section: Introductionmentioning

confidence: 99%

Dark matter imprint onB8neutrino spectrum

Lopes

Silk

2019

Phys. Rev. D

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The next generation of solar neutrino detectors will provide a precision measure of the 8 B electron-neutrino spectrum in the energy range from 1-15 MeV. Although the neutrino spectrum emitted by 8 B β-decay reactions in the Sun's core is identical to the neutrino spectrum measured in the laboratory, due to vacuum and matter flavor oscillations, this spectrum will be very different from that measured on Earth by the different solar neutrino experiments. We study how the presence of dark matter (DM) in the Sun's core changes the shape of the 8 B electron-neutrino spectrum. These modifications are caused by local variations of the electronic density and the 8 B neutrino source, induced by local changes of the temperature, density and chemical composition. Particularly relevant are the shape changes at low and medium energy range (E ν ≤ 10 MeV), for which the experimental noise level is expected to be quite small. If such a distortion in the 8 Bν e spectrum were to be observed, this would strongly hint in favor of the existence of DM in the Sun's core. The 8 B electron-neutrino spectrum provides a complementary method to helioseismology and total neutrino fluxes for constraining the DM properties. In particular, we study the impact of light asymmetric DM on solar neutrino spectra. Accurate neutrino spectra measurements could help to determine whether light asymmetric DM exists in the Sun's core, since it has been recently advocated that this type of DM might resolve the solar abundance problem.

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Stability of fundamental couplings: A global analysis

Cited by 34 publications

References 66 publications

Millisecond pulsars modeled as strange quark stars admixed with condensed dark matter

Millisecond pulsars modeled as strange quark stars admixed with condensed dark matter

Probing spatial variation of the fine-structure constant using the CMB

Dark matter imprint onB8neutrino spectrum

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