Future stability of perfect fluids with extreme tilt and linear equation of state p = c2 s for the Einstein-Euler system with positive cosmological constant: The range

• Grigorios Fournodavlos ^[1] ; Elliot Marshall ^[2] ; Todd A. Oliynyk ^[2]
  1. [1] University of Crete

     University of Crete

     Dimos Heraklion, Grecia

     
  2. [2] Monash University

     Monash University

     Australia

     
• Localización: Selecta Mathematica, New Series, ISSN 1022-1824, Vol. 32, Nº. 1, 2026
• Idioma: inglés
• DOI: 10.1007/s00029-025-01124-8
• Enlaces
  • Texto completo
• Resumen

  • We study the future stability of cosmological fluids, in spacetimes with an accelerated expansion, which exhibit extreme tilt behavior, i.e. their fluid velocity becoming asymptotically null at timelike infinity. It has been predicted in the article [17] that the latter behavior is dominant for sound speeds beyond radiation cs = 1/√3, hence,bifurcating off of the stable orthogonal fluid behavior modeled by the classical FLRWfamily of solutions, for c2s ∈[0, 1/3 ]. First, we construct homogeneous solutions to the Einstein-Euler system with the latter behavior, in S3 spatial topology, for sound speeds c2s ∈ ( 1/3 , 1). Then, we study their future dynamics and prove a global stability result in the restricted range c2s ∈ ( 1/3 , 37 ). In particular, we show that extreme tilt behavior persists to sufficiently small perturbations of the homogeneous backgrounds, without anysymmetry assumptions or analyticity. Our method is based on a bootstrap argument, in weighted Sobolev spaces, capturing the exponential decay of suitable renormalized variables. Extreme tilt behavior is associated with a degeneracy in the top order energy estimates that we derive, which allows us to complete our bootstrap argument only in the aforementioned restricted range of sound speeds. Interestingly, this is a degeneracy that does not appear in the study of formal series expansions. Moreover, for the Euler equations on a fixed FLRW background, our estimates can be improved to treat the entire beyond radiation interval c2s ∈ ( 1/3 , 1), a result already obtained in [21]. The latter indicates that the former issue is related to the general inhomogeneous geometry of the perturbed metric in the coupled to Einstein case.

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