deletions | additions       diff --git a/WH_YIS_THIS_PARA_WIDER__.tex b/WH_YIS_THIS_PARA_WIDER__.tex  index bad9826..779dfbb 100644  --- a/WH_YIS_THIS_PARA_WIDER__.tex  +++ b/WH_YIS_THIS_PARA_WIDER__.tex 
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For stars without suppressed modes (open circles), we can only derive an  upper limit to the field at the hydrogen-burning shell; above or below the shell the field could potentially be larger.   Considering first the low-mass stars ($< 1.1$\msol), we see from Figure 4 that magnetic fields above $10 \, {\rm kG}$ are not present at the hydrogen-burning shell when the stars are near the red giant luminosity bump (\numax\ $\sim50 \, \mu{\rm Hz}$). (HOW DOES THIS LOOK?)  Assuming magnetic flux conservation from the main-sequence phase, this suggests that magnetic fields above $1 \, {\rm kG}$ do not exist within the cores of Sun-like stars. This does not rule out, out  strong horizontal fields near the radiative-convective boundary because these fields are outside the core and cannot cause mode suppression when the star evolves into a red giant. %For stars with suppressed modes we derive the lower limit of how  %strong the field in the core [at least] needs to be for suppression to