deletions | additions       diff --git a/Considering_again_the_low_mass__.tex b/Considering_again_the_low_mass__.tex  index f49344b..d72fc4a 100644  --- a/Considering_again_the_low_mass__.tex  +++ b/Considering_again_the_low_mass__.tex 
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Considering again the low-mass stars ($< 1.1$\msol), of which none show  suppression, we see from Figure 4 that {\bf radial}  magnetic fields above $\approx 100 \, {\rm kG}$ are not present at the hydrogen-burning shell when the stars are  just below the red giant luminosity bump (\numax\ $\approx 70-100 \,  \mu{\rm Hz}$).  
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radiative-convective boundary because those fields would be outside the  core and could not cause mode suppression when the star evolves into a red  giant.