The term 'α-meteoroid' was introduced to describe a group of micrometeoroids with certain dynamical properties, which-alongside the group of the β-meteoroids-had been identified by the first generation of reliable in-situ dust detectors in interplanetary space. In recent years, use of the term α-meteoroid has become more frequent again, under a subtly but crucially altered definition. This work shall bring attention to the discrepancy between the term's original and newly established meaning, and spotlight the now-overlooked group of particles that the term used to describe. We review past and present pertinent literature around the term α-meteoroid, and assess the dynamics of the originally referred-to particles with respect to possible sources, showing that their formation is the expected consequence of collisional grinding of the zodiacal cloud at short heliocentric distances. The abundance of the original α-meteoroids, which are essentially 'bound β-meteoroids', makes them relevant to all in-situ dust experiments in the inner solar system. Due to the change of the term's meaning, however, they are not considered by contemporary studies. The characterization of this particle population could elucidate the processing of the innermost zodiacal cloud, and should thus be objective of upcoming in-situ dust experiments. The attained ambiguity of the term α-meteoroid is not easily resolved, warranting great care and clarity going forward.