In an attempt to interpret the observed properties of small scale magnetic fields at the solar surface, a set of models has been calculated based on the assumption of a magnetostatic equilibrium. The basic assumptions made are:

1. i. The observed magnetic elements are magnetostatic flux tubes.

2. ii. The efficiency of convective heat transport inside the tube is reduced with respect to that in the normal convection zone; the horizontal convective heat transport in the tube is suppressed completely by the magnetic field.

3. iii. Close to the tube, horizontal convective heat transport is reduced due to the proximity of the magnetic field.