  We calculate the quasinormal modes (QNM) frequencies of a test massless
scalar field and an electromagnetic field around static black holes in $f(T)$
gravity. Focusing on quadratic $f(T)$ modifications, which is a good
approximation for every realistic $f(T)$ theory, we first extract the
spherically symmetric solutions using the perturbative method, imposing two
ans$\ddot{\text{a}}$tze for the metric functions, which suitably quantify the
deviation from the Schwarzschild solution. Moreover, we extract the effective
potential, and then calculate the QNM frequency of the obtained solutions.
Firstly, we numerically solve the Schr$\ddot{\text{o}}$dinger-like equation
using the discretization method, and we extract the frequency and the time
evolution of the dominant mode applying the function fit method. Secondly, we
perform a semi-analytical calculation by applying the WKB method with the Pade
approximation. We show that the results for $f(T)$ gravity are different
compared to General Relativity, and in particular we obtain a different slope
and period of the field decay behavior for different model parameter values.
Hence, under the light of gravitational-wave observations of increasing
accuracy from binary systems, the whole analysis could be used as an additional
tool to test General Relativity and examine whether torsional gravitational
modifications are possible.
