[en] The Acapulco meteorite fell in August, 1976, at El Quemado, near Acapulco, Mexico. It is a unique object with chondritic composition but achondritic texture. High degree of recrystallisation and mineral chemical data indicate formation of the meteorite under redox conditions intermediate between those of H- and E-chondrites at approximately 1100⁰C, from which it cooled at a rate > 10⁰C/Myr. The major element composition is within the range of H-chondrites. Troilite and metal, and associated trace elements, are inhomogeneously distributed. Chromium is a factor of two higher than in H-chondrites. Enrichments of P and U indicate high phosphate content. Limited extent of partial melting may explain the light REE enrichment. However other incompatible elements have normal H-chondritic abundances or are even depleted like K and Rb. Moderately volatile or volatile elements (e.g. Mn, Ga, Ge, Zn) are enriched nearly to the level of C1-chondrites. Planetary noble gases are also significantly higher than in equilibrated ordinary chondrites. High temperature recrystallisation has not affected volatile element abundances. Compared to H-chondrites Acapulco is enriched in refractory siderophile elements. Low K and high U contents are also reflected in the anomalous amounts of ⁴⁰Ar and ⁴He. The old K-Ar age (4.7 +-0.3 Gyr) and high ²⁴⁴Pu track densities indicate mobilisation of U and Pu-rich phases shortly after formation of the parent material. An exposure age of 5 x 10⁶ yr is deduced from spallogenic rare gas data. (author)