deletions | additions       diff --git a/We_quantify_the_mass_dependence__.tex b/We_quantify_the_mass_dependence__.tex  index a829b62..8163001 100644  --- a/We_quantify_the_mass_dependence__.tex  +++ b/We_quantify_the_mass_dependence__.tex 
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convectively driven dynamos in the cores of at least some hydrogen-core burning (main-sequence)  stars. This agrees well with theoretical predictions based on 3D hydrodynamical modeling of the cores of main-sequence stars \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 have survived long after the dynamo terminated at the end of hydrogen-core burning in order to be detected during the red giant phase. Therefore, dynamo-generated fields are frequently able to settle into long-lived stable configurations (\citealt{Braithwaite_2004,Braithwaite_2006,Duez_2010}), a result that was not certain from the 3D hydrodynamical simulations.(HOW DOES THIS LOOK?)  % 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.