Abstract
We consider the cosmological relaxation of the Higgs mass and the cosmological constant due to the four-form fluxes in four dimensions. We present a general class of models with a singlet scalar field containing four-form couplings where the Higgs mass is relaxed to a right value and the Universe reheats to a sufficiently high reheating temperature after the last membrane nucleation. We also discuss some of interesting features in the cases of singlet scalar fields with non-minimal or minimal couplings to gravity and show how the new scalar fields can play a role for dark matter production.
Highlights
The relaxation mechanism with four-form fluxIn addition to the relaxation of the cosmological constant with four-form fluxes, the Higgs mass parameter is scanned at the same time
Both the non-minimal four-form coupling to gravity and the four-form coupling to a pseudoscalar inflaton [17] were considered by the same author to show that a successful chaotic inflation with spontaneously broken shift symmetry is achieved [18]
We present a general class of models with a singlet scalar field containing four-form couplings where the Higgs mass is relaxed to a right value and the Universe reheats to a sufficiently high reheating temperature after the last membrane nucleation
Summary
In addition to the relaxation of the cosmological constant with four-form fluxes, the Higgs mass parameter is scanned at the same time. For c2 = O(1) and the membrane charge e of electroweak scale, we can explain the observed Higgs mass parameter once the flux change stops at q = qc − e by the previous argument for the tunneling probability [11, 12]. In order to get Λeff (qc − e) to the observed value, we only have to tune the bare cosmological constant Λ against the flux contribution at the time of the last membrane nucleation. If the flux parameter and the membrane charge are variable for a tunable cosmological constant in the other vacua, the Higgs mass would not come right as observed. We will discuss some explicit examples for the inflaton potential
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