Dark energy without fine tuning. (arXiv:1905.00045v1 [gr-qc])
<a href="http://arxiv.org/find/gr-qc/1/au:+Camargo_Molina_J/0/1/0/all/0/1">José Eliel Camargo-Molina</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Markkanen_T/0/1/0/all/0/1">Tommi Markkanen</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Scott_P/0/1/0/all/0/1">Pat Scott</a>
We present a two-field model that realises inflation and the observed density
of dark energy today, whilst solving the fine-tuning problems inherent in
quintessence models. One field acts as the inflaton, generically driving the
other to a saddle-point of the potential, from which it acts as a quintessence
field following electroweak symmetry breaking. The model exhibits essentially
no sensitivity to the initial value of the quintessence field, naturally
suppresses its interactions with other fields, and automatically endows it with
a small effective mass in the late Universe. The magnitude of dark energy today
is fixed by the height of the saddle point in the potential, which is dictated
entirely by the scale of electroweak symmetry breaking.
We present a two-field model that realises inflation and the observed density
of dark energy today, whilst solving the fine-tuning problems inherent in
quintessence models. One field acts as the inflaton, generically driving the
other to a saddle-point of the potential, from which it acts as a quintessence
field following electroweak symmetry breaking. The model exhibits essentially
no sensitivity to the initial value of the quintessence field, naturally
suppresses its interactions with other fields, and automatically endows it with
a small effective mass in the late Universe. The magnitude of dark energy today
is fixed by the height of the saddle point in the potential, which is dictated
entirely by the scale of electroweak symmetry breaking.
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