Dimensionless constants, cosmology and other dark matters
Dimensionless constants, cosmology and other dark matters
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无量纲常数、宇宙学和其他暗物质
DOI：
10.1103/physrevd.73.023505
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发表时间：
2005
影响因子：
5
通讯作者：
F. Wilczek
中科院分区：
文献类型：
--
作者：
M. Tegmark;A. Aguirre;M. Rees;F. Wilczek
我们确定了粒子物理学和宇宙学所需的31个无量纲物理常数，并强调微物理约束和选择效应可能有助于阐明它们的起源。轴子宇宙学提供了一个有启发性的例子，在这个例子中，这两种论证都必须考虑在内，并且很好地协同工作。如果Peccei-Quinn相变发生在暴胀之前或暴胀期间，那么轴子暗物质密度将随概率分布而变化。通过计算净暗物质晕形成率作为所有四个相关的宇宙学参数的函数，并评估其他约束条件，我们发现，这种概率分布，计算在稳定的太阳系，可以说是达到峰值附近观察到的暗物质密度。如果发现了与宇宙学相关的弱相互作用大质量粒子（WIMP）暗物质，那么人们自然会期望WIMP和轴子的密度相当，这使得后续的精确测量非常重要，以确定WIMP是否可以解释所有的暗物质或仅仅是其中的一部分。
We identify 31 dimensionless physical constants required by particle physics and cosmology, and emphasize that both microphysical constraints and selection effects might help elucidate their origin. Axion cosmology provides an instructive example, in which these two kinds of arguments must both be taken into account, and work well together. If a Peccei-Quinn phase transition occurred before or during inflation, then the axion dark matter density will vary from place to place with a probability distribution. By calculating the net dark matter halo formation rate as a function of all four relevant cosmological parameters and assessing other constraints, we find that this probability distribution, computed at stable solar systems, is arguably peaked near the observed dark matter density. If cosmologically relevant weakly interacting massive particle (WIMP) dark matter is discovered, then one naturally expects comparable densities of WIMPs and axions, making it important to follow up with precision measurements to determine whether WIMPs account for all of the dark matter or merely part of it.