In this paper, we investigate the effects of varying bulk viscosity coefficients $\zeta(t)=\zeta_{ 0}+\zeta_{ 1}H$ on cosmic evolution within the framework of $f(T)$ teleparallel gravity. We focus on two cases: (i) $\zeta_{ 1} \neq0$ and (ii) $\zeta_{ 1} =0$, deriving the Hubble parameter $H$ as a function of redshift $z$ using a linear $f(T)$ model ($f(T) = \alpha T$ where $\alpha \neq 0$). Using the combined $H(z)+Pantheon^{ +}+BAO$ dataset, we obtain observational constraints on model parameters. For Case I ($\zeta_1 \neq 0$), best-fit values are $H_0=60.0^{ +2.0}_{ -1.9}$ km/s/Mpc, $\alpha=1.01^{ +0.10}_{ -0.098}$, $\zeta_0=40.1^{ +1.9}_{ -2.0}$, and $\zeta_1=0.123^{ +0.093}_{ -0.088}$, while for Case II ($\zeta_1 = 0$), they are $H_0=67.5^{ +1.3}_{ -1.3}$ km/s/Mpc, $\alpha=0.94^{ +0.14}_{ -0.13}$, and $\zeta_0=34.7^{ +2.0}_{ -2.0}$. The analysis reveals a transition in the deceleration parameter, indicating a shift from deceleration to acceleration of the universe's expansion, with present-day values of $q_{ 0} \approx -0.49$ and $q_{ 0} \approx -0.32$ for the respective cases. The jerk parameter $j(z)$ and effective EoS for the cosmic viscous fluid also support the cosmic acceleration, with trajectories aligning with the quintessence scenario. These findings underscore the potential of our $f(T)$ model dominated by bulk viscous matter in explaining cosmic acceleration.
Categories: astro-ph.CO gr-qc