Serra de Magé is clearly of cumulative origin, based on its texture and the distribution of incompatible elements, as shown by the evident positive anomaly of the Eu. The high U-Rb ratio and the anortite content indicates that his parental body was, or relatively high in refractory elements or low in moderately volatile lithophiles. Low-pressure fusion experiments on eucrite-type meteorites, carried out by Stolper (1977), demonstrated that the Serra de Magé may have been formed from liquids produced by an extensive fractionation of advanced partial fusions from regions supplying eukritic liquids instead of liquids similar composition. On the other hand, Consolmagno & Drake (1977), using information collected by Stolper (1977), abundance of rare earth elements and some assumptions, concluded that the meteorite originated from accumulation from liquids produced by an extensive fractionation of pyroxene and plagioclase . A detailed investigation of the Serra de Magé pyroxene shows that it initially crystallized as pigeonite, but during the slow cooling, augite exhaustion and inversion to hyperstene occurred. A cooling rate of 4x10-4 ºC / year and a depth of approximately 5 km was estimated for the formation of the Serra de Magé. Source: Gomes & Keil (1980).