Configurational entropy in $f(T)$ gravity
  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 $f(T) = \zeta (-T)^ b$, where, $\zeta = (6
H_{0}^{2})^{(1-s)}\frac{\Omega_{P_{0}}}{2 s -1}$ 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.
