论文标题
解释哈勃张力起源的现象学模型
Phenomenological model explaining Hubble Tension origin
论文作者
论文摘要
最近在宇宙学中揭示的问题之一是一种所谓的哈勃张力（HT），这是当前哈勃常数值之间的差异，通过在红移$ z \ Lessim 1 $上观察到宇宙，以及通过观察到具有$ z $ z \ z sim sim sim 1100 $的CMB波动的遥远的宇宙。 In this paper we suggest, that this discrepancy may be explained by deviation of the cosmological expansion from a standard Lambda-CDM %simple Friedman model of a flat universe, during the period after recombination at $z \lesssim 1100$, due to action of additional variable component of a dark energy of different origin.. We suppose, that a dark matter (DM) has a common origin with a variable component of a dark energy (DEV). DE目前可能有两个组件，其中一个是爱因斯坦常数$λ$，另一个较小的组件开发（$λ_v$）来自负责通货膨胀的标量场的残余。由于共同的起源和互连，DEV和DM的密度应该被连接，并且至少在重组后的时间几乎保持恒定，当时我们可能会近似$ρ_{dm} =αρ_{dev} $。黑暗能量的这一部分与宇宙常数$λ$没有相关，而是由存在量度可变的标量字段所定义的。考虑到开发人员对宇宙扩展的影响，我们发现$α$的值可能消除了HT问题。为了在$ z <1100 $的时间间隔内保持几乎恒定的DEV/DM能量密度比，我们建议存在较宽的质量DM粒子分布。
One of the problem revealed recently in cosmology is a so-called Hubble tension (HT), which is the difference between values of the present Hubble constant, measured by observation of the universe at redshift $z \lesssim 1$, and by observations of a distant universe with CMB fluctuations originated at $z \sim 1100$. In this paper we suggest, that this discrepancy may be explained by deviation of the cosmological expansion from a standard Lambda-CDM %simple Friedman model of a flat universe, during the period after recombination at $z \lesssim 1100$, due to action of additional variable component of a dark energy of different origin.. We suppose, that a dark matter (DM) has a common origin with a variable component of a dark energy (DEV). DE presently may have two components, one of which is the Einstein constant $Λ$, and another, smaller component DEV ($Λ_V$) comes from the remnants of a scalar fields responsible for inflation. Due to common origin and interconnections the densities of DEV and DM are supposed to be connected, and remain almost constant during, at least, the time after recombination, when we may approximate $ρ_{DM}=αρ_{DEV}$. This part of the dark energy in not connected with the cosmological constant $Λ$, but is defined by existence of scalar fields with a variable density. Taking into account the influence of DEV on the universe expansion we find the value of $α$ which could remove the HT problem. In order to maintain the almost constant DEV/DM energy density ratio during the time interval at $z<1100$, we suggest an existence of a wide mass DM particle distribution.
