$f(T)$引力中的解析熵
Configurational entropy in $f(T)$ gravity
摘要：
宇宙构型熵的演化依赖于密度涨落的增长率和哈勃参数。本文研究了幂律$f(T)$引力模型的组态熵演化，其中$ζ= (6 H_{0}^{2})^{(1-s)}\frac{Ω_{P_{0}}}{2 s -1}$和$b$为自由参数。从分析中，我报告说，在$f(T)$引力的组态熵是负的，并随着增加的标度因子，因此与加速宇宙一致。当$b$消失时，构型熵的降低最大，因为当$b=0$时，暗能量的影响最大。此外，我发现，随着参数$b$的增加，增长率，增长模式，和物质密度参数的演变缓慢，而哈勃参数的演变迅速。哈勃参数的快速演化与$b=0$的增长率相结合，可以为构型熵的大耗散提供解释。
英文摘要：
The evolution of the configurational entropy of the universe relies on the growth rate of density fluctuations and on the Hubble parameter. In this work, I present the evolution of configurational entropy for the power-law $f(T)$ gravity model of the form $f(T) = ζ(-T)^ b$, where, $ζ= (6 H_{0}^{2})^{(1-s)}\frac{Ω_{P_{0}}}{2 s -1}$ and $b$ a free parameter. From the analysis, I report that the configurational entropy in $f(T)$ gravity is negative and decreases with increasing scale factor and therefore consistent with an accelerating universe. The decrease in configurational entropy is the highest when $b$ vanishes since the effect of dark energy is maximum when $b=0$. Additionally, I find that as the parameter $b$ increases, the growth rate, growing mode, and the matter density parameter evolve slowly whereas the Hubble parameter evolves rapidly. The rapid evolution of the Hubble parameter in conjunction with the growth rate for the $b=0$ may provide an explanation for the large dissipation of configurational entropy.
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