Abstract: The coalescence of a binary system of neutron stars represents a perfect scenario to study hot and ultra-dense matter. Under these extreme conditions, exotic species such as hyperons may be present too. In this seminar I will speak about the influence that the appearance of hyperons have on the equation of state, and consequently, the signatures they may leave in the observables measured from the astrophysical phenomena. In particular, I will focus on the signatures that come from the thermal behaviour of hyperons in matter. The presence of hyperons produces a significant drop of the thermal pressure. This effect consequently induces a characteristic increase of the dominant postmerger gravitational-wave frequency by up to ∼ 150 Hz compared to purely nucleonic EoS models.