A Test of the Supernova Trigger Hypothesis with [TSUP]60[/TSUP]F[CLC]e[/CLC] and [TSUP]26[/TSUP]A[CLC]l[/CLC]

It is shown that if the 26 Al inventory of the early solar system, taken as ( 26 Al/ 27 Al) =5 × 10 −5 , is a result of injection of fresh debris from a Type II supernova (SNII), then 60 Fe/ 56 Fe would have to be between 3 × 10 −7 and 1 × 10 −5 . This inferred correlation of 26 Al and 60 Fe is based on the observation that both nuclei are produced dominantly in the O/Ne zone and that for SNII ejecta 26 Al/ 60 Fe is between 0.6 and 23. A similar correlation applies to 41 Ca, 36 Cl, 16 O, and 18 O, which are also produced in the same zone or in nearby regions. The supernova trigger hypothesis may be tested by determination of 60 Ni excesses correlated with Fe in samples where 26 Al was demonstrated to be present. From available experimental data, it appears that the observed abundance of 60 Fe is too low to be compatible with a supernova trigger that injected the 26 Al into the protosolar nebula. The same is true for 53 Mn, a short-lived nucleus produced in the outer edge of the Ni core.