Erratum: Looking for axion dark matter in dwarf spheroidal galaxies [Phys. Rev. D 
<b>98</b>
, 083024 (2018)]

Caputo, Andrea; Garay, Carlos Peña; Witte, Samuel J.

doi:10.1103/physrevd.99.089901

Cited by 32 publications

(19 citation statements)

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“…Currently there is a large number of researchers that study several phenomenological implications of the axion, both in astrophysics and cosmology and for an important stream of research articles on this timely issue see for example [21, and references therein. Also there are currently many experiments running and theoretical studies that may verify the existence of µeV or even much smaller masses for the axion [71][72][73][74][75][76][77][78][79] with most of these experiments and theoretical proposals invoking the axion photon conversion in a magnetic field [80][81][82]. In addition, the future LISA collaboration may reveal axionic effects coming from gravitational waves related to superradiance of black holes [50][51][52].…”

Section: Introductionmentioning

confidence: 99%

Geometric inflation and dark energy with axion F(R) gravity

2020

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We present a model of F (R) gravity in the presence of a string theory motivated misalignment axion like particle materialized in terms of a canonical scalar field minimally coupled with gravity, and we study the cosmological phenomenology of the model, emphasizing mainly on the late-time era. The main result of the paper is that inflation and the dark energy era may be realized in a geometric way by an F (R) gravity, while the axion is the dark matter constituent of the Universe. The F (R) gravity model consists of an R 2 term, which as we show dominates the evolution during the early time, thus producing a viable inflationary phenomenology, and a power law term ∼ R δ with δ ≪ 1 and positive, which eventually controls the late-time era. The axion field remains frozen during the inflationary era, which is an effect known for misalignment axions, but as the Universe expands, the axion starts to oscillate, and its energy density scales eventually as we show, as ρa ∼ a −3 . After appropriately rewriting the gravitational equations in terms of the redshift z, we study in detail the late-time phenomenology of the model, and we compare the results with the ΛCDM model and the latest Planck 2018 data. As we show, the model for small redshifts 0 < z < 5 is phenomenologically similar to the ΛCDM model, however at large redshifts and deeply in the matter domination era, the results are different from those of the ΛCDM model due to the dark energy oscillations. For the late-time study we investigate the behavior of several well-known statefinder quantities, like the deceleration parameter, the jerk and Om(z), and we demonstrate that the statefinders which contain lower derivatives of the Hubble rate have similar behavior for both the ΛCDM and the axion F (R) gravity model. We conclude that the axion F (R) gravity model can unify in a geometric way the inflationary epoch with the dark energy era, and with the axion being the main dark matter constituent.PACS numbers: 04.50. Kd, 95.36.+x, 98.80.Cq,

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Section: Introductionmentioning

confidence: 99%

Geometric inflation and dark energy with axion F(R) gravity

2020

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“…So far, only a small part of the QCD axion parameter space has been explored due to its weak interaction with matter [22,23]. However, new experimental techniques to search for axions have been recently proposed [24][25][26][27][28][29][30][31][32][33][34][35] (see Ref. [36] for a comprehensive review).…”

Section: Introduction -mentioning

confidence: 99%

Unique Multimessenger Signal of QCD Axion Dark Matter

et al. 2020

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We propose a multi-messenger probe of the natural parameter space of QCD axion dark matter based on observations of black hole-neutron star binary inspirals. It is suggested that a dense dark matter spike may grow around intermediate mass black holes (10 3 − 10 5 M ). The presence of such a spike produces two unique effects: a distinct phase shift in the gravitational wave strain during the inspiral and a enhancement of the radio emission due to the resonant axion-photon conversion occurring in the neutron star magnetosphere throughout the inspiral and merger. Remarkably, the observation of the gravitational wave signal can be used to infer the dark matter density and, consequently, to predict the radio emission. We study the projected sensitivity to the axion-photon coupling in the light of the LISA interferometer and next-generation radio telescopes such as the Square Kilometre Array. Given a sufficiently nearby detection, such observations will explore the QCD axion in the mass range 10 −7 eV to 10 −5 eV.

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“…For this purpose, we solve the coupled Freidmann equations for the radion field (ξ(t)) and the scale factor (a(t)) during initial era and the solutions are given in eqns. (39) and (40)) respectively. It is demonstrated in Fig.…”

Section: Resultsmentioning

confidence: 99%

“…Using the solutions of ξ(t), a(t) (see eqns. (39), (40)) along with the estimated values of the parameters (v v , h 0 , ξ 0 ), we give the plots for the interbrane separation (T (t), see figure [4]) and the deceleration parameter (q = −ä/a, see figure [5]) against a dimensionless time variablet = t t f N . where we use the relation ξ(t) = 24M 3 k e −kπT (t) .…”

Section: Parametersmentioning

confidence: 99%

Dynamical suppression of spacetime torsion

Paul

SenGupta

2019

Eur. Phys. J. C

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A surprising feature of our present four dimensional universe is that its evolution appears to be governed solely by spacetime curvature without any noticeable effect of spacetime torsion. In the present paper, we give a possible explanation of this enigma through "cosmological evolution" of spacetime torsion in the backdrop of a higher dimensional braneworld scenario. Our results reveal that the torsion field may had a significant value at early phase of our universe, but gradually decreased with the expansion of the universe. This leads to a negligible footprint of torsion in our present visible universe. We also show that at an early epoch, when the amplitude of the torsion field was not suppressed, our universe underwent through an inflationary stage having a graceful exit within a finite time. To link the model with observational constraints, we also determine the spectral index for curvature perturbation (ns) and tensor to scalar ratio (r) in the present context, which match with the results of P lanck 2018 (combining with BICEP-2 Keck-Array) data [1].

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Erratum: Looking for axion dark matter in dwarf spheroidal galaxies [Phys. Rev. D 98 , 083024 (2018)]

Cited by 32 publications

References 0 publications

Geometric inflation and dark energy with axion F(R) gravity

Geometric inflation and dark energy with axion F(R) gravity

Unique Multimessenger Signal of QCD Axion Dark Matter

Dynamical suppression of spacetime torsion

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