Interacting dark energy with CPL admits exact solutions via incomplete gamma functions; Q proportional to dark energy density modestly improves AIC fit but BIC prefers LambdaCDM, showing phantom-to-quintessence transition and possible future transient acceleration.
Coupled quintessence
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Decaying dark matter is mapped to a scalar field model that requires phantom dark energy and is reinterpreted via a complex scalar with ultra-light mass to form a unified dark fluid whose phantom phase is a stable late-time attractor.
New cosmological data mildly favor a small coupling between dark matter and a scalar dark energy field at |β| ≈ 0.03 while allowing an effective phantom-crossing equation of state.
citing papers explorer
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Cosmological evolution of interacting dark energy with a CPL equation of state
Interacting dark energy with CPL admits exact solutions via incomplete gamma functions; Q proportional to dark energy density modestly improves AIC fit but BIC prefers LambdaCDM, showing phantom-to-quintessence transition and possible future transient acceleration.
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Correspondence between a decaying dark matter sector scenario and scalar field model
Decaying dark matter is mapped to a scalar field model that requires phantom dark energy and is reinterpreted via a complex scalar with ultra-light mass to form a unified dark fluid whose phantom phase is a stable late-time attractor.
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Constraints on Coupled Dark Energy in the DESI Era
New cosmological data mildly favor a small coupling between dark matter and a scalar dark energy field at |β| ≈ 0.03 while allowing an effective phantom-crossing equation of state.