  The recent discovery by Cayrel et al. of U in CS 31082-001 along with Os and
Ir at greatly enhanced abundances but with [Fe/H]=-2.9 strongly reinforces the
argument that there are at least two kinds of SNII sources for r-nuclei. One
source is the high-frequency H events responsible for heavy r-nuclei (A>135)
but not Fe. The H-yields calculated from data on other ultra-metal-poor stars
and the sun provide a template for quantitatively predicting the abundances of
all other r-elements. In CS 31082-001 these should show a significant
deficiency at A<135 relative to the solar r-pattern. It is proposed that CS
31082-001 should have had a companion that exploded as an SNII H event. If the
binary survived the explosion, this star should now have a compact companion,
most likely a stellar-mass black hole. Comparison of abundance data with
predicted values and a search for a compact companion should provide a
stringent test of the proposed r-process model. The U-Th age determined by
Cayrel et al. for CS 31082-001 is, to within substantial uncertainties, in
accord with the r-process age determined from solar system data. The time gap
between Big Bang and onset of normal star formation only allows r-process
chronometers to provide a lower limit on the age of the universe.
