deletions | additions       diff --git a/MAYBE_REMOVE_NEXT_PARAGRAPH_AND__.tex b/MAYBE_REMOVE_NEXT_PARAGRAPH_AND__.tex  index f11f01f..0af504b 100644  --- a/MAYBE_REMOVE_NEXT_PARAGRAPH_AND__.tex  +++ b/MAYBE_REMOVE_NEXT_PARAGRAPH_AND__.tex 
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evolve towards lower \numax. % This trend is also evident in Fig.1.   Most stars fall on the ``normal'' upper branch of $V^2\approx 1.5$, in  agreement with previous results \citep{Mosser_2011}.   The lower branch with suppressed dipole modes, agrees remarkably well with theoretical predictions (black curve). This reduction assumes that all the wave energy leaking into the stellar core is trapped. According The suppression occurs because wave energy leaking into the core is trapped due to a magnetic greenhouse effect caused by strong internal magnetic fields (Fuller et al. 2015).  %According  to theoretical work (Fuller et al. 2015), this occurs in stars with %with  strong internal magnetic fields. For this branch the decrease of the suppression towards lower \numax\ is a consequence of the increasingly weaker coupling between acoustic waves in the envelope and gravity waves in the core as stars evolve (Fuller et al. 2015). With this large stellar sample we can separate the stars into five different mass intervals, represented in Fig.2 from 0.9 to 2.1\msol, which clearly shows that the relative  population on the lower branch (stars with suppressed dipole modes) is strongly mass dependent.