deletions | additions       diff --git a/We_quantify_the_mass_dependent__.tex b/We_quantify_the_mass_dependent__.tex  index bf6eaa9..9921447 100644  --- a/We_quantify_the_mass_dependent__.tex  +++ b/We_quantify_the_mass_dependent__.tex 
...
We quantify the mass-dependent mode suppression mass-dependence  in Fig. 3 by showing the relative number ofstars with  suppressed dipole modes stars  (those below the dashed line in Fig. 2) in narrow mass intervals.   We see no stars with reduced power suppression  in the dipole modes stars  below 1.1\msun, while above this threshold there  is first a gradual increase followed by a rapid increase above approximately  1.5\msun, and a drop beyond 2.0\msun.   The onset of suppression beyond 1.1\msun, 1.1\msun.   This  coincides with the mass above below  which stars are thought to do not  form convective cores during their hydrogen-core burning phase \citep{Kippenhahn_1990}. We believe The onset of magnetic suppression above  this shows evidence for threshold suggests  the establishment existence  of convectively driven dynamos in the cores of at least some  hydrogen-core burning stars that are only 10-20\% more massive than the Sun   \citep{Charbonneau_2001,MacGregor_2003,Brun_2005}. (main-sequence)  stars. This agrees well with theoretical predictions based on 3D hydrodynamical modeling   \citep{Brun_2005}.  %[THE SENTENCE BEFORE AND AFTER DONT REALLY WORK TOGTHER BUT I FEEL WE NEED TO SAY SOMEHOW WHAT IS SAID IN THE FOLLOWING SENTENCE]  The resulting strong magnetic fields must survive long after the dynamo terminates at the end of hydrogen-core burning in order to be detected during the red giant phase. phase; [REPHRASE REST OF SENTENCE OR REMOVE] a results that was not certain from the 3D hydrodynamical simulations.  % The gradual increase in suppression may result from the increasing size of  % the convective core in more massive stars, which generates stronger  % magnetic fields that survive after hydrogen burning ceases in the core.   % [Jim/Matteo elaborate?]  Stars above $1.6 M_\odot$ show a 50-60\% suppression rate, much larger than  can be accounted for by the up to 10\% of A-type stars known to show strong surface fields,  \citep{2008CoSka..38..443P}. This shows