REVIEW 4 cited by
Interacting Quintessence, Cosmic Acceleration and the Coincidence Problem
Not yet reviewed by Pith; the record is open.
This paper has not been read by Pith yet. Machine review is queued; the pith claim, tier, and objections will appear here once it completes.
SPECIMEN: schema-true, not a live event
T0 review · schema-true
One-sentence machine reading of the paper's core claim.
pith:XXXXXXXX · record.json · timestamp
abstract
Faced by recent evidence for a flat universe dominated by dark energy, cosmologists grapple with deep cosmic enigmas such as the cosmological constant problem, extreme fine-tuning and the cosmic coincidence problem. The extent to which we observe the dimming of distant supernovae suggests that the cosmic acceleration is as least as severe as in cosmological constant models. Extrapolating this to our cosmic future implies terrifying visions of either a cold and empty universe or an explosive demise in a ``Big Rip.'' We construct a class of dynamical scalar field models of dark energy and dark matter. Within this class we can explain why supernovae imply a cosmic equation of state $w\lesssim-1$, address fine tuning issues, protect the universe from premature acceleration and predict a constant fraction of dark energy to dark matter in the future (thus solving the coincidence problem), satisfy the dominant energy condition, and ensure that gravitationally bound objects remain so forever (avoid a Big Rip). This is achieved with a string theory inspired Lagrangian containing standard kinetic terms, exponential potentials and couplings, and parameters of order unity.
Forward citations
Cited by 4 Pith papers
-
Evolving Dark Sector and the Dark Dimension Scenario
A two-parameter fading dark sector model, with exponential dark energy potential and exponential dark matter mass, matches DESI DR2 plus supernova data and naturally yields apparent w<-1 phantom behavior.
-
Solving an Interacting Quintessence Model with a Sound Horizon Initial Condition and its Observational Constraints
An interacting quintessence model with initial conditions set by the CMB sound horizon angle increases H0 with coupling strength, but observational constraints show it does not resolve the H0 or S8 tensions.
-
Interacting Scalar Fields as Dark Energy and Dark Matter in Einstein scalar Gauss Bonnet Gravity
Interacting scalar fields coupled to Gauss-Bonnet gravity yield viable dark energy and dark matter models that match Pantheon+ and DES supernova data while preferring over LambdaCDM at high redshifts with Roman mocks.
-
Topological defects as effective dynamical dark energy
A few percent domain-wall component gives a mild (Δχ² = -1.72) improvement over ΛCDM when fitting DESI DR2 BAO and DESY5 supernovae, but the evidence is inconclusive.
Discussion (0). Sign in to comment.