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Gradient instability for w < -1

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arxiv astro-ph/0406043 v3 pith:ZZ63DEYI submitted 2004-06-01 astro-ph gr-qchep-phhep-th

classification astro-phgr-qchep-phhep-th
keywords signbackgroundeffectivekineticlagrangianspatialtermcases
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abstract

We show that in single scalar field models of the dark energy with equations of state satisfying $w \equiv p / \rho < -1$, the effective Lagrangian for fluctuations about the homogeneous background has a wrong sign spatial kinetic term. In most cases, spatial gradients are ruled out by microwave background observations. The sign of $w+1$ is not connected to the sign of the time derivative kinetic term in the effective Lagrangian.

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Forward citations

Cited by 4 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Geodesic completeness of anisotropic cosmologies and the null energy condition

    gr-qc 2026-08 conditional novelty 7.0 of 10

    A Bianchi-I spacetime obeying the null energy condition and expanding in all directions at one time must have past-incomplete null geodesics.

  2. Monodromic Dark Energy and DESI

    astro-ph.CO 2025-07 conditional novelty 6.0 of 10

    Monodromic k-essence fits current CMB, BAO, and supernova data about as well as w0-wa dark energy, with a nonzero oscillation amplitude preferred only by DESY5 supernovae.

  3. Energy conditions of bouncing solutions in quadratic curvature gravity coupled with a scalar field

    gr-qc 2026-03 unverdicted novelty 4.0 of 10

    Bouncing solutions in quadratic curvature gravity with a scalar field satisfy null, weak, and dominant energy conditions but violate the strong one when using the scalar-field energy-momentum tensor, while all four co...

  4. Restoration of the Lorentz symmetry of particle propagator in the ghost condensate model

    gr-qc 2025-09 conditional novelty 3.0 of 10

    Choosing the Lorentz-violating tensor with spatial components Bii = -3B00 makes the quadratic kinetic term Lorentz invariant, giving the phantom excitation the dispersion omega^2 = k^2 for any background.

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