For two interacting scalar fields, low-energy ghosts are equivalent to tachyonic instabilities and high-energy ghosts to gradient instabilities, with rare cases where interactions stabilize two ghosts.
First, we define the phas e space variables as: Q = φ k, P = ∂ L ∂ ˙φ k = K ˙φ k, (13) and obtain the Hamiltonian density H : H = 1 2 P2 K + 1 2 M2Q2
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Cosmological Instabilities and the Role of Matter Interactions in Dynamical Dark Energy Models
For two interacting scalar fields, low-energy ghosts are equivalent to tachyonic instabilities and high-energy ghosts to gradient instabilities, with rare cases where interactions stabilize two ghosts.