Hope is the sum of goal thoughts as tapped by pathways and agency. Pathways reflect the perceived capability to produce goal routes; agency reflects the perception that one can initiate action along these pathways. Using trait and state hope scales, studies explored hope in college student athletes. In Study 1, male and female athletes were higher in trait hope than nonathletes; moreover, hope significantly predicted semester grade averages beyond cumulative grade point average and overall self-worth. In Study 2, with female cross-country athletes, trait hope predicted athletic outcomes; further, weekly state hope tended to predict athletic outcomes beyond dispositional hope, training, and self-esteem, confidence, and mood. In Study 3, with female track athletes, dispositional hope significantly predicted athletic outcomes beyond variance related to athletic abilities and affectivity; moreover, athletes had higher hope than nonathletes.A typical dictionary definition of hope as "a desire and the confident expectation of its fulfillment" captures one of the fundamental reasons that humans enjoy sporting activities (Osterhoudt, 1978). From the First Olympiad in 776 B.C. to neighborhood basketball games to next year's Super Bowl, the athletes' hopes for desired sport goals are pivotal to understanding these activities. Nevertheless, the role of hope has remained unexplored among personality researchers interested in individual differences in motivation, as well as by sport psychologists, largely because a theoretical model of hope and the associated measurement instruments have not been available. Accordingly, on the basis of the recent development of a theory of hope and measurement indices related to this construct, the present series of studies was performed to provide initial information about the role of hope in the academic and sport achievements of college students.Previously, scholarly writings have defined hope as a unidimensional construct involving an overall perception that goals can be met (French, 1952;Lewin, 1935;Stotland, 1969). Expanding on this unidimensional model, Snyder and his col-

A dying massive star ends in a supernova explosion ejecting a large fraction of its mass into the interstellar medium. If this happens nearby, part of the ejecta might end on Solar System bodies and, in fact, radioactive ^{60}Fe has been detected on the Pacific ocean floor in about 2 Ma old layers. Here, we report on the detection of this isotope also in lunar samples, originating presumably from the same event. The concentration of the cosmic ray produced isotope ^{53}Mn, measured in the same samples, proves the supernova origin of the ^{60}Fe. From the ^{60}Fe concentrations found we deduce a reliable value for the local interstellar fluence in the range of 1×10^{8}  at/cm^{2}. Thus, we obtain constraints on the recent and nearby supernova(e).

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60 Fe must have been injected into the protosolar nebula and mixed to less than 10% heterogeneity before formation of planetary bodies.

We measured the Ni isotopic composition of metal from a variety of meteorite groups to search for variations in the 60Ni abundance from the decay of the short-lived nuclide 60Fe (t(1/2) = 1.49 My) and for possible nucleosynthetic effects in the other stable isotopes of Ni. We developed a high-yield Ni separation procedure based on a combination of anion and cation exchange chromatography. Nickel isotopes were measured on a single-focusing, multicollector, inductively coupled mass spectrometer (MC-ICPMS). The external precision on the mass-bias-corrected 60Ni/58Ni ratio (+/-0.15 epsilon; 2sigma) is comparable to similar studies using double-focusing MC-ICPMS. We report the first high-precision data for 64Ni, the least abundant Ni isotope, obtained via MC-ICPMS. The external precision on the mass-bias-corrected 64Ni/58Ni ratio (+/-1.5 epsilon; 2sigma) is better than previous studies using thermal ionization mass spectrometry. No resolvable excesses relative to a terrestrial standard in the mass-bias-corrected 60Ni/58Ni ratio were detected in any meteoritic metal samples. However, resolvable deficits in this ratio were measured in the metal from several unequilibrated chondrites, implying a 60Fe/56Fe ratio of approximately 1 x 10(-6) at the time of Fe/Ni fractionation in chondritic metal. A 60Fe/56Fe ratio of (4.6 +/- 3.3) x 10(-7) is inferred at the time of Fe/Ni fractionation on the parent bodies of magmatic iron meteorites and pallasites. No clearly resolvable non-mass-dependent anomalies were detected in the other stable isotopes of Ni in the samples investigated here, indicating that the Ni isotopic composition in the early solar system was homogeneous (at least at the level of precision reported here) at the time of meteoritic metal formation.