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tokens: H i Ly α (lower left), low-TZ Si iii 1206 Å (upper left), low-TZ C iii 1175 Å (lower right), and coronal soft X-rays (upper right). These flux–flux diagrams are more populated given the better FUV coverage of the two stars, although the C iii comparison for B is still missing points for epochs when E140H exposures were taken: these cut off just below Si iii 1206 Å, so C iii 1175 Å was excluded. As tentatively seen in the Mg ii panels previously, the A correlations line up nicely with the solar equivalents, although A’s X-rays still are shifted downward, and noisier than the others perhaps partly because of non-simultaneous coverage. Again, there is somewhat disjoint behavior in several of the panels between the A and B relations. Notice also that A’s Ly α slope closely matches that of the solar correlation, but B’s trend is somewhat shallower. Similarly, the Si iii correlation against C ii is noticeably shallower for B, and curiously shifted downward, compared to A or the Sun. At the same time, the C iii behavior of B appears to be steeper. Finally, A’s X-rays (though scattered) seem to show a steeper rise with increasing C ii , as in the lower branch of the Sun’s bent power law, whereas B displays a flatter relation (although still with α ∼ 2). Figure 16 (c) displays correlations between low-TZ Si iii 1206 Å and low-TZ C iii 1175 Å (lower left), mid-TZ Si iv 1400 Å (upper left), mid-TZ C iv 1550 Å (lower right), and mid-TZ N v 1240 Å (upper right). Again, the C iii comparison is lacking a few points for α Cen B, most conspicuously on the low-flux side. Despite that, all four panels have the same general appearance: the A points closely track the translated solar power laws, while B shows universally steeper slopes. Curiously, the B trends have “retreated” backward to the extent that the A and B origins of the four correlations are similar (again taking into account the abbreviated C iii series for B). This is a consequence of the behavior seen in the upper left panel of Figure 16 (b), wherein B’s Si iii points are seen to parallel those of A, but also approach a similar minimum. This behavior is unlike the other diagnostics shown earlier, for which the minimum B value generally was comparable to, or exceeded, that of A’s maximum. The contrary behavior emphasizes the unique position of Si iii 1206 Å in both the Sun and α Cen A, as a “super-active” species, showing the steepest power laws relative to the other FUV features, even including hot N v . In α Cen B, in contrast, the Si iii feature has declined in strength, and shows the expected “stellar” behavior, namely Si iv , C iv , and especially N v all exhibit power laws comparable or steeper than unity against Si iii . The final figure, Figure 16 (d), illustrates a number of miscellaneous, but nonetheless illuminating, comparisons. The lower left panel compares the two Mg ii resonance lines, which are both affected by ISM absorptions, but the k-line more so than the weaker