deletions | additions       diff --git a/We_quantify_the_mass_dependence__.tex b/We_quantify_the_mass_dependence__.tex  index 453a608..2472cf6 100644  --- a/We_quantify_the_mass_dependence__.tex  +++ b/We_quantify_the_mass_dependence__.tex 
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which stars do not form convective cores during their hydrogen-core burning phase \citep{Kippenhahn_1990}.  The onset of magnetic suppression above this threshold suggests the existence of  convectively driven magnetic dynamos in the cores of at least some hydrogen-core burning (main-sequence)  stars. stars, as shown in 3D hydrodynamical modeling of the cores of main-sequence stars \citep{Brun_2005}.  Red giants do not contain convective cores, therefore we conclude the strong fields in suppressed oscillators are the remnants of the fields produced by core dynamos during the main sequence. %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 \citep{Braithwaite_2004,Braithwaite_2006,Duez_2010}, a result that was not certain from the 3D hydrodynamical simulations.