The reconstruction of tachyon inflationary potentials

Qin, Fei; Gong, Yungui; Lin, Jiong; Zhu, Yanjun

doi:10.1088/1475-7516/2017/08/018

Cited by 29 publications

(40 citation statements)

References 47 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…These considerations make this description of dark energy an interesting alternative to both fluid and canonical scalar field models. The tachyon models have also been extensively studied in the context of inflation [42][43][44][45][46][47][48][49]. Since tachyon scalar field shows dust like equation of state in its cosmic evolution, the 'tachyon dust' is considered as a potential candidate of combined dark energy and dark matter [36,37,[50][51][52][53][54].…”

Section: Introductionmentioning

confidence: 99%

Low redshift observational constraints on tachyon models of dark energy

Singh

Sangwan

Jassal

2019

J. Cosmol. Astropart. Phys.

View full text Add to dashboard Cite

The background evolution of an accelerated, dark energy dominated universe is aptly described by non-canonical tachyon scalar field models. The accelerated expansion of the universe is determined by the choice of a suitable scalar field potential; in the case of a tachyon field, a 'runaway' potential. In the absence of a fundamental theory, dark energy properties are studied in a phenomenological approach. This includes determining the model parameters using observations and to probe the allowed deviation from the cosmological constant model. In this paper, we present constraints on tachyon scalar field parameters from low redshift data for two different scalar field potentials. These scalar field potentials have been crucial in tachyon dark energy studies. The datasets considered in this paper include the supernova type Ia data, independent measurements of the Hubble parameter and the Baryon Acoustic Oscillation data. In this paper, we present constraints on tachyon field parameters using these observations and their combination. A combination of the datasets indicates that those model parameters are preferred which emulate the cosmological constant model. The initial value of the scalar field, in the unit of the Hubble constant, is bounded from below and does not require fine-tuning at larger values.

show abstract

Section: Introductionmentioning

confidence: 99%

Low redshift observational constraints on tachyon models of dark energy

Singh

Sangwan

Jassal

2019

J. Cosmol. Astropart. Phys.

View full text Add to dashboard Cite

show abstract

“…Another interesting feature of our work is that the value of the scalar field for which the graceful exit occurs, coincides with the inflection point of the scalar potential, a feature which can be interesting phenomenologically. Several authors support the idea of an inflection point in the potential generating reheating [60,62,70,78,85].…”

Section: Discussionmentioning

confidence: 91%

Canonical scalar field inflation with a Woods–Saxon potential

Oikonomou

Chatzarakis

2019

Annals of Physics

View full text Add to dashboard Cite

This paper focuses on the realization of an inflationary model from a canonical scalar field theory with a Woods-Saxon potential, in the slow-roll approximation. Our analysis indicates that the observable quantities derived theoretically from our model, namely the spectral index of the primordial scalar curvature perturbations and the tensor-to-scalar ratio, are compatible with the latest Planck collaboration data. We also discuss the qualitative features of the potential, and we show that the value of the scalar field for which the graceful exit occurs, coincides with the inflection point of the scalar potential. We also attempt to study the post-inflation reheating phase of the model, in order to further examine the viability of the Woods-Saxon scalar field model, and as we demonstrate the results indicate viability of the model for this era too, however the instantaneous reheating is not allowed for the model at hand. PACS numbers: 04.50. Kd, 95.36.+x, 98.80.Cq,

show abstract

“…To the leading order of 1/N, many inflation models have the universal result n s = 1 − 2/N, they include the R 2 inflation [3] and the hilltop inflation [4], the Higgs inflation with the nonminimal coupling ξφ 2 R [5,6] also gives the same n s when ξ 1, which is a special case of the more general nonminimal coupling ξ f (φ)R with the potential λ 2 f 2 (φ) for an arbitrary function f (φ) in the strong coupling limit ξ 1 [7]. The above relation between n s and N can be generalized to the parametrization of the observables in terms of N and used to reconstruct inflationary potential [8][9][10][11][12][13][14][15][16][17][18][19].…”

Section: Introductionmentioning

confidence: 85%