deletions | additions       diff --git a/It_may_be_interesting.tex b/It_may_be_interesting.tex  index b8d71c8..03ab9b8 100644  --- a/It_may_be_interesting.tex  +++ b/It_may_be_interesting.tex 
...
In contrast to the sub-surface FeCZ, convective cores  are prevalent in all stars above about 1.2$\mso$. It has been found  that the longer lifetime of stars of lower  mass may favor the drift of fields produced in the core to the surface \citep{1978A&A....68...57S,2003ApJ...586..480M}. \citep{1978AA....68...57S,2003ApJ...586..480M}.  Therefore, the expected trend is opposite to that found for fields produced  by the FeCZ, where surface fields may occur only for stars  above a critical mass (or luminosity), and stronger fields are found for  more massive stars.  On the other hand, in contrast to fields from the FeCZ,  magnetic flux tubes produced in the core may carry CNO-processed   material to the surface.  This might thus constitute a   mechanism to explaining nitrogen enrichment in slowly rotating  early~B stars \citep{Mba06,Mgb08,2008ApJ...676L..29H}.   Strong fossil magnetic fields are thought to persist   in only a fraction of massive stars   and may lead to, among other phenomena,  highly anomalous surface chemical compositions, wind confinement, and variable   X-ray emission \citep{2006AA...451..195W,2005ApJ...630L..81T}.   Those strong features can clearly not be produced by fields originating   from the FeCZs.  Finally, magnetic fields produced in differentially rotating massive stars by the  Spruit-Taylor dynamo \citep{Spr02}   may transport angular momentum and chemical species \citep{hws05}.  These fields are predominantly of toroidal geometry and would quickly decay near the stellar surface,  and are thus not thought to lead to observable fields at the stellar surface (but see also \citet{2005MNRAS.356.1139M}).