deletions | additions       diff --git a/Bfield.tex b/Bfield.tex  index a74da6f..698f3fa 100644  --- a/Bfield.tex  +++ b/Bfield.tex 
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Second, the stellar wind could be threaded by a stellar magnetic field. Fields on YSOs are often quite complex with a mixture of open and closed field lines \citep[e.g.][]{2011MNRAS.417..472D,2012MNRAS.425.2948D} and their configuration changes in coronal activity.  Qualitatively, closed field lines can either fill with coronal plasma or connect to the accretion disk and carry accretion funnels. Only those parts of the stellar surface connected to open field lines can launch a wind. Thus, the total mass loss rate would be reduced compared to a spherical wind that we assume here.   As a simple estimate we calculate the magnetic pressure $P_{\textrm{mag}}=\frac{\vec B^2}{8 $P_{\textrm{mag}}=\frac{\boldsymbol{B}^2}{8  \pi}$ for a split monopole field with a field strength of 1~kG at $r=R_\odot$ and compare it to the ram presure (eqn.~\ref{eqn:Pofz}). Using the fiducial parameters from Table~\ref{tab:fiducial} the ram presure dominates over the magnetic pressure already at 0.1~AU and since $P_{\textrm{mag}} \propto \vec B^2 \boldsymbol{B}^2  \propto r^{-4}$, while $P_\{textrm{ram}} $P_{\textrm{ram}}  \propto r^{-2}$ (eqn.~\ref{eqn:Pofz} and \ref{eqn:rho}) we can neglect the magnetic presure of the stellar wind for our model.