Nonminimal torsion-matter coupling extension of<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>f</mml:mi><mml:mo stretchy="false">(</mml:mo><mml:mi>T</mml:mi><mml:mo stretchy="false">)</mml:mo></mml:math>gravity

Harkó, Tiberiu; Lobo, Francisco S. N.; Otalora, Giovanni; Saridakis, Emmanuel N.

doi:10.1103/physrevd.89.124036

Cited by 192 publications

(178 citation statements)

References 78 publications

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“…The resulting f (T, T ) theory is different from f (T ) gravity, from the curvature-based f (R, T ) gravity [83], as well as from the recently constructed nonminimally torsion-matter coupled theory where T is coupled to the matter Lagrangian L m instead of T [99]. Therefore, it is a novel modified gravitational theory.…”

Section: Discussionmentioning

confidence: 79%

“…The incorporation of non-minimally coupled scalar-torsion theories was performed in [90][91][92][93][94][95][96][97][98], where a scalar field couples non-minimally to the torsion scalar T . Similarly, in [99] nonminimally matter-torsion theories were constructed, where the matter Lagrangian is coupled to a second f (T ) function. We mention that both these scenarios are different than the corresponding curvature ones, despite the fact that uncoupled GR coincides with TEGR.…”

Section: Contents 1 Introductionmentioning

confidence: 99%

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f(T,𝒯) gravity and cosmology

Harkó

Lobo

Otalora

et al. 2014

J. Cosmol. Astropart. Phys.

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259

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Abstract. We present an extension of f (T ) gravity, allowing for a general coupling of the torsion scalar T with the trace of the matter energy-momentum tensor T . The resulting f (T, T ) theory is a new modified gravity, since it is different from all the existing torsion or curvature based constructions. Applied to a cosmological framework, it leads to interesting phenomenology. In particular, one can obtain a unified description of the initial inflationary phase, the subsequent non-accelerating, matter-dominated expansion, and then the transition to a late-time accelerating phase. Additionally, the effective dark energy sector can be quintessence or phantom-like, or exhibit the phantom-divide crossing during the evolution. Moreover, in the far future the universe results either to a de Sitter exponential expansion, or to eternal power-law accelerated expansions. Finally, a detailed study of the scalar perturbations at the linear level reveals that f (T, T ) cosmology can be free of ghosts and instabilities for a wide class of ansatzes and model parameters.

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Section: Discussionmentioning

confidence: 79%

Section: Contents 1 Introductionmentioning

confidence: 99%

f(T,𝒯) gravity and cosmology

Harkó

Lobo

Otalora

et al. 2014

J. Cosmol. Astropart. Phys.

Self Cite

259

213

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“…(For a review, see Refs. [6][7][8][9][10][11][12][13] In this model, due to the tiny DM particle mass m = O (10 −22 )eV, the DM particle number density is very high and hence the inter-particle distance is much smaller than the de Broglie wave length of the DM particles. Therefore, the particles are in BEC and move collectively as a wave rather than incoherent particles.…”

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confidence: 99%

Brief History of Ultra-light Scalar Dark Matter Models

Lee

2018

EPJ Web Conf.

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Abstract. This is a review on the brief history of the scalar field dark matter model also known as fuzzy dark matter, BEC dark matter, wave dark matter, or ultra-light axion. In this model ultra-light scalar dark matter particles with mass m = O(10 −22 )eV condense in a single Bose-Einstein condensate state and behave collectively like a classical wave. Galactic dark matter halos can be described as a self-gravitating coherent scalar field configuration called boson stars. At the scale larger than galaxies the dark matter acts like cold dark matter, while below the scale quantum pressure from the uncertainty principle suppresses the smaller structure formation so that it can resolve the small scale crisis of the conventional cold dark matter model.Despite long efforts dark matter (DM) remains a great mystery in physics and astronomy [1]. While numerical results of the cold dark matter (CDM) model are remarkably successful in explaining the large scale structure of the universe, it encounters some problems at the scale of galactic or sub-galactic structures. For example, the numerical simulations usually predict cusped central halo density and too many sub-halos and small galaxies, which seem to be in contradiction with observations [2][3][4][5].Recently, there is a growing interest in the idea that DM particles are ultra-light scalars in Bose-Einstein condensate (BEC). (For a review, see Refs. 6-13) In this model, due to the tiny DM particle mass m = O(10 −22 )eV, the DM particle number density is very high and hence the inter-particle distance is much smaller than the de Broglie wave length of the DM particles. Therefore, the particles are in BEC and move collectively as a wave rather than incoherent particles. At the scale larger than galaxies the DM perturbation behaves like that of CDM, while below the scale quantum pressure from the uncertainty principle suppresses the small structure formation, which makes it a viable alternative to CDM. This property helps us to resolve the small scale problems of the CDM model such as the missing satellite problem or the cusp/core problem [14].Before 2000 there were only a few groups of scientists working on this topic, without much communication even between them. Being unaware of precedent works, many researchers in this field independently proposed similar ideas with various names such as BEC DM, scalar field DM (SFDM), fuzzy DM, ultra-light axion (ULA), ultralight axion like particle (ALP), wave DM, ψ DM, repulsive DM or (super)fluid DM among many, although the basic physics of these models is quite similar. (Henceforth, I will use the term 'SFDM' for the model.) This unfortunate ⋆ e-mail: scikid@jwu.ac.kr situation has brought some confusions among researchers in this field. Therefore, at this point, it is desirable to summarize what have already attempted in this exciting field. 1The hypothesis that galactic DMs are ultra-light scalar particles in BEC has a long history. In Ref.[15] Baldeschi et al. considered the galactic halo model of self-gravitating bosons wit...

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“…In fact the above scale factor and similar ones, e.g. [48], can be obtained as a subclass of a more generalized family of scale factors, calledq-de Sitter [64], whereq is a free parameter. This scale factor is an intermediate form between power-law and de Sitter, where both dark energy and dark matter simultaneously are described by this family of solutions.…”

Section: Modified Friedmann Equationsmentioning

confidence: 99%

“…In contrast, the f (T ) theories cannot be conformally equivalent to TEGR plus a scalar field [27]. Short period these pioneering studies have been followed by a large number of works exploring different aspects of the f (T ) gravity in astrophysics [28][29][30][31][32][33][34][35][36][37][38][39][40] and in cosmology [41][42][43][44][45][46][47][48][49][50][51][52][53][54][55][56]. Some applications show interesting results, e.g.…”

Section: B F (T ) Gravitymentioning

confidence: 99%

The hidden flat like universe II

Hanafy

Nashed

2016

Astrophys Space Sci

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In a recent work, a particular class of f (T ) gravity, where T is the teleparallel torsion scalar, has been derived. This class has been identified by flat-like universe (FLU) assumptions [1]. The model is consistent with the early cosmic inflation epoch. A quintessence potential has been constructed from the FLU f (T )-gravity. We show that the first order potential of the induced quintessence is a quasi inverse power law inflation with an additional constant providing an end of the inflation with no need to an extra mechanism. At e-folds N * = 55 before the end of the inflation, this type of potential can perform both E and B modes of the cosmic microwave background (CMB) polarization pattern.

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Nonminimal torsion-matter coupling extension off(T)gravity

Cited by 192 publications

References 78 publications

f(T,𝒯) gravity and cosmology

f(T,𝒯) gravity and cosmology

Brief History of Ultra-light Scalar Dark Matter Models

The hidden flat like universe II

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