of massive and low-mass stars. The heavier stable isotopes 84,86 Kr are also subject to a substantial contribution from the r process (see [6] for a recent estimate). On the other hand, two of its lighter isotopes, 80,82 Kr, shielded from the r process by 80,82 Se, are pure s-process nuclides making their natural abundances [7-9] solid anchors for the validation of s-process models (see [6] and references therein). The determination of Kr solar abundances via analysis of primitive meteorites (C1 carbonaceous chondrites) is, however, difficult, and Kr isotopic composition in meteorites is considered a prominent anomalous case in the s-process pattern [10,11]. The few Kr measurements on acid residues of SiC presolar grains [12] have been theoretically interpreted as a mix between solar material and nucleosynthesis products of asymptotic giant branch (AGB) stars [13].