The very-metal-poor halo star CS 31082-001 was discovered to be very strongly r-process-enhanced during the course of a VLT+UVES high-resolution follow-up of metal-poor stars identified in the HK survey of Beers & colleagues .
Both the strong n-capture element enhancement and the low carbon and nitrogen content of the star ( reducing the CN molecular band contamination ) led to the first ^ { 238 } U abundance measurement in a stellar spectrum ( Cayrel et al .
2001 ) , and the opportunity to use both radioactive species ^ { 238 } U and ^ { 232 } Th for dating the progenitor to this star .
However , age computations all rely on the hypothesis that the r-process pattern is solar , as this was indeed observed in the other famous r-process-enhanced very metal poor stars CS 22892-052 ( Sneden et al .
1996 , 2000 ) and in HD 115444 ( Westin et al .
2000 ) .
Here , we investigate whether this hypothesis is verified also for CS 31082-001 , using a preliminary analysis of over 20 abundances of n-capture elements in the range Z=38 to Z=92 .