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Quintessential inflation with canonical and noncanonical scalar fields and Planck 2015 results
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We investigate two classes of models of quintessential inflation, based upon canonical as well as noncanonical scalar fields. In particular, introducing potentials steeper than the standard exponential, we construct models that can give rise to a successful inflationary phase, with signatures consistent with Planck 2015 results. Additionally, using nonminimal coupling of the scalar field with massive neutrino matter, we obtain the standard thermal history of the Universe, with late-time cosmic acceleration as the last stage of evolution. In both cases, inflation and late-time acceleration are connected by a tracker solution.
Forward citations
Cited by 7 Pith papers
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Cosmological Constraints on Neutrino Masses in Quintessential Inflation
In the α-attractor quintessential-inflation scenario, Planck PR4 + DESI DR2 BAO + Pantheon+ supernova data imply Σmν < 0.067 eV (flat) and <0.116 eV (with curvature).
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Scaling solutions in quintessential inflation
In quintessential inflation, the scalar field misses the scaling-solution attractor during radiation, so a single exponential tail can drive both inflation and dark energy.
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Observational constraints on early time non-phantom behaviour of dynamical dark energy
Early scaling dark energy is constrained to be less than about one percent at matter-radiation equality and is disfavored by model selection, while late-time CPL dynamics show only a weak preference away from ΛCDM.
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Forecasting constraints on quintessential inflation from future generation of galaxy and CMB surveys
Future CMB and galaxy surveys are forecast to constrain the alpha-attractor quintessential inflation parameter to alpha = 2 ± 0.17 and the spectral index to n_s = 0.965 ± 0.0014.
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Baryogenesis in the paradigm of quintessential inflation
Quintessential inflation can generate the observed baryon asymmetry through a derivative coupling of the inflaton to a non-conserved baryon current, at the price of a carefully chosen cutoff scale.
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The Wave Function of the Universe and Inflation
Rearranging the Wheeler-DeWitt equation defines the inflaton potential in terms of an arbitrary wave-function phase and amplitude; nothing constrains that wave function, so the potential is relabeled rather than deriv...
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The Scale Factor Potential Approach to Inflation
The paper reparametrizes slow-roll inflation through a scale factor potential and constructs an example potential, but the chosen 60 e-fold branch is inconsistent with its own first-minimum end condition.
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