Isocurvature Perturbations in Quintessence Cosmologies

Details Isocurvature Perturbations in Quintessence Cosmologies Isocurvature Perturbations in Quintessence Cosmologies

2003-10-09

arxiv.org/abs/gr-qc/0310052v1

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

Talk given at the Blois '03 Conference on Cosmology

Scientific paper

We present a systematic treatment of the initial conditions and evolution of cosmological perturbations in a universe containing photons, baryons, neutrinos, cold dark matter, and a scalar quintessence field. By formulating the evolution in terms of a differential equation involving a matrix acting on a vector comprised of the perturbation variables, we can use the familiar language of eigenvalues and eigenvectors. As the largest eigenvalue of the evolution matrix is fourfold degenerate, it follows that there are four dominant modes with non-diverging gravitational potential at early times, corresponding to adiabatic, cold dark matter isocurvature, baryon isocurvature and neutrino isocurvature perturbations. We conclude that quintessence does not lead to an additional independent mode.

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