The term magnetic flux cancellation describes a dynamic phenomena involving the interaction of opposite polarity magnetic features resulting in their subsequent flux removal from the solar surface. Cancellation occurs frequently in the active and the quiet regions of the Sun over a wide range of spatial and temporal scales. It is a key process that removes magnetic flux from the photosphere, thereby maintaining the surface flux budget. Cancellation also play a significant role in many of the upper atmospheric dynamic phenomena and is supposed to be a contributor to upper atmospheric heating as well. Small-scale, short-lived magnetic features that carry a substantial amount of magnetic flux are ubiquitous on the solar surface. In this talk, I will present spectropolarimetric observations of cancellation events involving such small-scale, short-lived magnetic features in an active- and a quiet region. I will then discuss the characteristics of these events,mainly in the solar photosphere.