The Stability Issue In Models Of Neutrino Dark Energy

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Presentation transcript:

The Stability Issue In Models Of Neutrino Dark Energy by Ole Bjælde with A. Brookfield, C. van de Bruck, S. Hannestad, D. Mota, L. Schrempp, & D. Tocchini-Valentini Wednesday 22-08-07 Cosmo07 Brighton

Mass Varying Neutrinos =MaVaNs Coupling between  and a scalar field  Conservation of energy Equations of motion Fardon, Nelson & Weiner, 2003

Assuming adiabaticity MaVaNs Mass Varying Neutrinos =MaVaNs NR limit Assuming adiabaticity

MaVaNs MaVaN- candidates Candidate potentials must obey w~-1

MaVaNs Coleman-Weinberg

MaVaNs Power-Law

Cosmological Perturbation Theory Evolution of structures from Big Bang Perturbations grow because of gravity

Stability Dynamics of perturbations governed by General sound speed described by MaVaNs Adiabatic scale

Stability Stable MaVaN model-perturbations driven by Generalising to 3 neutrino generations with a degenerate mass spectrum Takahashi & Tanimoto, 2003

Perturbation Analysis Perturbations Perturbation Analysis Synchronous gauge Friedmann Neutrino-e.o.m.

Results Results: C-W

Results Results: Power

Conclusion MaVaNs can act as dark energy Dynamics of MaVaN-perturbations depend crucially on  Instability in cases of steeply growing  It is possible to have a stable model! Ridiculeously small growth in neutrino mass