暴胀和精粹的有效标量场理论中来自不同质量尺度的功率抑制
Power suppression from disparate mass scales in effective scalar field theories of inflation and quintessence
摘要：
一个标量势耦合到其他大的不同质量的场，将表现出这些大质量场的量子回路校正的功率抑制。暗能量体系中的精粹场和暴胀过程中的暴胀子场通常具有非常大的背景场值。因此，任何其他场，其质量通过适度耦合依赖于精粹/暴胀子背景场值，在暗能量/暴胀阶段将变得非常大，其对标量有效势的量子修正将被抑制。本文利用解耦定理提出了这一概念。这个问题就归结为在耦合常数、标量场背景值和重整化标度的参数空间中抑制效应大小的定量问题。文中给出了暴胀场和精粹场的一些数值例子，但该方法是通用的，可以应用于任何标量场有效势。这里发展的退耦效应对暗能量的影响是，精粹场不需要仅仅是一个令人难以置信的弱相互作用场，通常只是作为一个附加物来产生暗能量，没有其他目的。相反，这个精粹场可能在早期的粒子物理动力学中发挥核心作用，然后在暗能量阶段开始之前的后期简单地去耦。对于暴胀，结果是暴胀子与其他场的耦合在某些模型中可以大得多，而不需要超对称来控制量子校正。
英文摘要：
A scalar potential coupled to other fields of large disparate masses will exhibit power suppression of the quantum loop corrections from these massive fields. Quintessence fields in the dark energy regime and inflaton fields during inflation often have a very large background field value. Thus any other field with its mass dependent on the quintessence/inflaton background field value through a moderate coupling will become very massive during the dark energy/inflation phase and its quantum corrections to the scalar effective potential will be suppressed. This concept is developed in this paper using the decoupling theorem. The problem then reduces to a quantitative question of the size of suppression effects within the parameter space of coupling constants, scalar field background value and renormalization scale. Some numerical examples are presented both for inflation and quintessence, but the approach is general and can be applied to any scalar field effective potential. The consequences to dark energy of the decoupling effect developed here is that the quintessence field need not just be an incredibly weakly interacting field, often added as simply an add-on to generate dark energy and have no other purpose. Instead, this quintessence field could play a central role in the particle physics dynamics at early times and then simply decouple at late times before the onset of the dark energy phase. For inflation a consequence is coupling of the inflaton to other fields can be much larger in certain models, without needing supersymmetry to control quantum corrections.
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