deletions | additions       diff --git a/WH_YIS_THIS_PARA_WIDER__.tex b/WH_YIS_THIS_PARA_WIDER__.tex  index 6ff2065..2971c02 100644  --- a/WH_YIS_THIS_PARA_WIDER__.tex  +++ b/WH_YIS_THIS_PARA_WIDER__.tex 
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For a given \numax\, stars more massive than 1.4\msol require increasingly strong magnetic fields to suppress their dipole modes. From Figure 4, there is no clear upper limit to the field strengths attainable in red giant cores, as suppressed stars are common even when field strengths $ B> 1 \, {\rm MG}$ are required for suppression. However, the hint of a fractional decline of suppressed stars beyond 2\msol seen in Fig. 3 suggests there may be an upper limit to the stellar mass beyond which typical dynamo-generated magnetic fields can no longer cause oscillation mode suppression in intermediate-mass stars. Such an upper mass limit may be caused by the differing core structure of stars more massive than 2\msol, which evolve through the red giant phase much faster than stars of lower mass.   The high occurrence rate of dipole mode suppression shows that core-dynamo-generated fields often remain stable through the red giant phase more than $10^8 \, {\rm yr}$ after the dynamo shuts off at the end of hydrogen-core burning. The occurrence rate of these long-lived core fields is much larger than the occurrence rate of strong fields observed at the surfaces of magnetic Ap stars, which may have been generated by a pre-hydrogen-core burning dynamo during star formation (e.g., \citealt{Moss_2004}). \citealt{Moss_2003}).  We conclude that fields generated during hydrogen-core burning are able to settle into stable equilibrium configurations much more commonly (greater than $60\%$ of the time) than fields generated during star formation (less than $10\%$ of the time). %JIM/MATTEO: HERE MORE STUFF RELATED TO THAT INCLUDING FIG 4b OF NUMBER OF NORMAL/SUPPRESSED