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The Little Rip
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The Little Rip
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We examine models in which the dark energy density increases with time (so that the equation-of-state parameter w satisfies w < -1), but w approaches -1 asymptotically, such that there is no future singularity. We refine previous calculations to determine the conditions necessary to produce this evolution. Such models can display arbitrarily rapid expansion in the near future, leading to the destruction of all bound structures (a "little rip"). We determine observational constraints on these models and calculate the point at which the disintegration of bound structures occurs. For the same present-day value of w, a big rip with constant w disintegrates bound structures earlier than a little rip.
Forward citations
Cited by 5 Pith papers
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Non-Hermitian Holographic Flows to Little Rip Cosmologies
A holographic model of a non-Hermitian PT-symmetric QFT produces black hole interiors that are isotropic Little Rip cosmologies, separated from standard Kasner behavior by a distinctive logarithmic signature in heavy-...
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A Spectrum of Cosmological Rips and Their Observational Signatures
A unified dark energy model with sigmoid correction generates a spectrum of rip futures that all fit DESI, Pantheon+, and CMB data at the same level as ΛCDM.
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$\Lambda$CDM-like models with future singularities
Dark energy models with pressure defined as a function of scale factor match ΛCDM observations today but develop finite-time future singularities, including exact scalar field representations and calculated effects on...
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Effective Phantom Dark Energy: What Cosmological Reconstruction Does and Does Not Imply
Effective phantom dark energy is a background-level reconstruction that does not imply fundamental pathologies such as ghost instabilities or null energy condition violation by the underlying stress tensor.
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Finite scale factor and future singularities
Dark energy models with pressure as a function of scale factor produce type I-IV finite-time future singularities that exhibit similar late-time behavior.
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