Constraining neutrino masses, the cosmological constant and BSM physics from the weak gravity conjecture
Constraining neutrino masses, the cosmological constant and BSM physics from the weak gravity conjecture
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弱引力猜想中的约束中微子质量、宇宙常数和 BSM 物理
DOI：
10.1007/jhep11(2017)066
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发表时间：
2017
影响因子：
5.4
通讯作者：
I. Valenzuela
中科院分区：
文献类型：
--
作者：
L. Ibáñez;Victor Martín;I. Valenzuela
我们知道存在AdS真空，它是通过将SM紧化为二维或三维而得到的。这种真空的存在取决于通过卡西米尔效应的中微子质量的值。利用弱引力猜想，最近Ooguri和Vafa论证了这样的真空与嵌入相容量子引力理论的SM不相容。我们研究了在没有这种危险的3D和2D SM AdS真空的情况下，宇宙学常数Λ4和中微子质量的极限。一个有趣的推论是Λ4有界大于mν4阶标度，正如实验所观察到的。有趣的是，这是第一个仅在粒子物理学基础上暗示Λ4不为零的论点，没有宇宙学的输入。相反，观测到的Λ4意味着对SM中中微子质量的强约束，也适用于一些BSM扩展，包括额外的Weyl或Dirac旋量，引力子和轴子。中微子质量的上界意味着（对于固定中微子Yukawa和Λ4）EW标度上存在上界。对于具有跷跷板机制的大质量马约拉纳中微子，其大尺度M为1010 − 14 GeV，Y为1 <$10 −3，我们得到EW尺度不能超过MEW <$102 − 104 GeV。从这个观点来看，为了得到一个小的EW尺度所需要的精细微调将是一个海市蜃楼，因为产生更高EW尺度的参数将处于沼泽地中，不会被视为可能的一致理论。这将为电子战等级问题带来新的视角。
A bstractIt is known that there are AdS vacua obtained from compactifying the SM to 2 or 3 dimensions. The existence of such vacua depends on the value of neutrino masses through the Casimir effect. Using the Weak Gravity Conjecture, it has been recently argued by Ooguri and Vafa that such vacua are incompatible with the SM embedding into a consistent theory of quantum gravity. We study the limits obtained for both the cosmological constant Λ4 and neutrino masses from the absence of such dangerous 3D and 2D SM AdS vacua. One interesting implication is that Λ4 is bounded to be larger than a scale of order mν4, as observed experimentally. Interestingly, this is the first argument implying a non-vanishing Λ4 only on the basis of particle physics, with no cosmological input. Conversely, the observed Λ4 implies strong constraints on neutrino masses in the SM and also for some BSM extensions including extra Weyl or Dirac spinors, gravitinos and axions. The upper bounds obtained for neutrino masses imply (for fixed neutrino Yukawa and Λ4) the existence of upper bounds on the EW scale. In the case of massive Majorana neutrinos with a see-saw mechanism associated to a large scale M ≃ 1010 − 14 GeV and Yν1 ≃ 10−3, one obtains that the EW scale cannot exceed MEW ≲ 102 − 104 GeV. From this point of view, the delicate fine-tuning required to get a small EW scale would be a mirage, since parameters yielding higher EW scales would be in the swampland and would not count as possible consistent theories. This would bring a new perspective into the issue of the EW hierarchy.
走出沼泽的缠绕：用F项缠绕膨胀规避弱引力猜想？
影响因子：
4.4
作者：
A. Hebecker;P. Mangat;F. Rompineve;L. T. Witkowski
通讯作者：
L. T. Witkowski
失控的放松单一性
影响因子：
5.4
作者：
L. McAllister;P. Schwaller;G. Servant;J. Stout;A. Westphal
通讯作者：
A. Westphal