Accretion of weak flux tubes into the EHM occurs in the SFMHD+MF simulation of Beckwith et al. (2009; left hand frame). Right hand frame: isolated flux tubes in the 3D radiatively inefficient simulations of (Igumenshchev 2008) and (Punsly et al. 2009). The strength of the vertical poloidal magnetic field is color coded. Dark blue is no field and red is a strong field (near equipartition with the gas pressure). The inner calculational boundary is a circle of radius 2M. Notice the weaker, green, small patches of vertical flux in the inner accretion flow. See the text for more details.