Fractional gravity yields stable de Sitter expansion and exact bouncing solutions driven by phantom (w < -1) or ghost (negative energy) fluids, with results independent of the form-factor representation.
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No CMB-consistent CPL dark energy model can simultaneously fit both the BAOtr and DESI datasets; the 3.7-sigma disagreement at z=0.51 sets an irreducible floor.
Re-expressing the Hubble tension via posterior-implied E(z) histories yields moderate mismatches (S_hist of 1.65 and 2.55) that correspond to only 1.1-2.1 sigma equivalents, below the usual 4.9 sigma scalar-H0 discrepancy.
Generalized interacting dark energy models with constant or dynamical couplings yield analytical density expressions but are not preferred over LambdaCDM by Bayesian evidence from DESI, Pantheon+, and CMB data.
citing papers explorer
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Cosmology of fractional gravity
Fractional gravity yields stable de Sitter expansion and exact bouncing solutions driven by phantom (w < -1) or ghost (negative energy) fluids, with results independent of the form-factor representation.
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On the origin of the BAOtr-DESI tension
No CMB-consistent CPL dark energy model can simultaneously fit both the BAOtr and DESI datasets; the 3.7-sigma disagreement at z=0.51 sets an irreducible floor.
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From Scalar $H_0$ to $E(z)$: A Reformulation of the Hubble Tension
Re-expressing the Hubble tension via posterior-implied E(z) histories yields moderate mismatches (S_hist of 1.65 and 2.55) that correspond to only 1.1-2.1 sigma equivalents, below the usual 4.9 sigma scalar-H0 discrepancy.
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Generalizing the CPL Parametrization through Dark Sector Interaction
Generalized interacting dark energy models with constant or dynamical couplings yield analytical density expressions but are not preferred over LambdaCDM by Bayesian evidence from DESI, Pantheon+, and CMB data.