  We study the emission of gravitational waves from spheroidal magnetized
strange stars for both an isolated slowly rotating star and a binary system. In
the first case, we compute the quadrupole moment and the amplitude of
gravitational waves that may be emitted. For the binary system, the tidal
deformability is obtained by solving simultaneously the system of spheroidal
structure equations and the Love number equation. These results are compared
with the data inferred from the GW170817 event which is also used to calculate
the mass and tidal deformability of the companion star in the binary system.
  Our model supports binary systems formed by magnetized strange stars
describing reasonable signals of gravitational waves contrasted with other
models of binary systems composed of magnetized hadronic stars and
non-magnetized quark stars.
