The Standard Model (SM) possesses an instability at high scales that would be catastrophic during or just after inflation, and yet no new physics has been seen to alter this. Furthermore, modern developments in quantum gravity suggest that the SM degrees of freedom are not unique; that a typical low energy effective theory should include a large assortment of hidden sector degrees of freedom. It is therefore puzzling that cosmological constraints from BBN and CMB reveal that the early universe was almost entirely dominated by the SM, when the inflaton $\phi$ could have decayed into many sectors. In this work we propose the following explanation for all of this: we allow the lowest dimension operators with natural coefficients between the inflaton and both the Higgs and hidden sectors. Such hidden sectors are assumed to be entirely natural; this means all unprotected masses are pushed up to high scales and project out of the spectrum, while only massless (or protected) degrees of freedom remain, and so the inflaton can only reheat these sectors through higher dimension (and suppressed) operators. On the other hand, the SM possesses a special feature: it includes a light Higgs $H$, presumably for life to exist, and hence it allows a super-renormalizable coupling to the inflaton $\phi H^\dagger H$, which allows rapid decay into the SM. We show that this naturally (i) removes the instability in the Higgs potential both during and after inflation due to a tree-level effect that increases the value of the Higgs self-coupling from the IR to the UV when one passes the inflaton mass, (ii) explains why the SM is dominant in the early universe, (iii) allows dark matter to form in hidden sector/s through subsequent dynamics (or axions, etc), (iv) allows for high reheating and baryogenesis, and (v) accounts for why there so far has been no direct detection of dark matter or new physics beyond the SM.

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解释早期宇宙为何稳定并受标准模型支配

标准模型 (SM) 在大尺度上具有不稳定性，这在暴胀期间或暴胀之后会是灾难性的，但尚未发现新的物理学可以改变这一点。此外，量子引力的现代发展表明，SM 自由度并不是唯一的。一个典型的低能量有效理论应该包括各种各样的隐藏扇区自由度。因此，令人费解的是，来自 BBN 和 CMB 的宇宙学约束表明，早期宇宙几乎完全由 SM 主导，当时暴胀子 $\phi$ 可能已经衰变为许多扇区。在这项工作中，我们对所有这些提出以下解释：我们允许在暴胀子与希格斯和隐藏扇区之间具有自然系数的最低维算子。这种隐藏的扇区被认为是完全自然的；这意味着所有未受保护的质量都被推到高尺度并投射到光谱之外，而只剩下无质量（或受保护的）自由度，因此暴胀子只能通过更高维（和抑制）的算子重新加热这些扇区。另一方面，SM 拥有一个特殊的特征：它包含一个轻的希格斯 $H$，推测生命存在，因此它允许超重整化耦合到暴胀子 $\phi H^\dagger H$，其中允许快速衰减到 SM。我们表明，这自然地（i）消除了暴胀期间和暴胀后希格斯势能的不稳定性，这是由于树级效应增加了当一个人通过暴胀子质量时从红外到紫外光的希格斯自耦合值， (ii) 解释了为什么 SM 在早期宇宙中占主导地位，