What can we learn from the r - element distribution of CS 22892 - 052 ?

The striking similarity between the solar distribution of r-element abundances in the 56 ≤ Z ≤ 76 range and the corresponding abundance pattern observed in the ultra-metalpoor star CS 22892-052 is analysed. It is found that such an observation does not necessarily imply that the whole A >∼ 70 distribution of r-nuclides, including Th, suspected to have been engulfed in CS 22892-052 at the same time as the detected elements is solar. Such a conclusion derives from the finding that an arbitrary superposition of r-process events that does not fit the whole solar r-process pattern can also account for the CS 22892-052 observations. The interpretation of this result and its implications are discussed.