  The radial structure of accretion disks is a fundamental issue regarding star
and planet formation. Many theoretical studies, focussing on different aspects
such as e.g. disk emissivity or ionization, have been conducted in the context
of the Standard Accretion Disk (SAD) model, where no jet is present. We wish to
calculate the structure of YSO accretion disks in an approach that takes into
account the presence of the protostellar jets. The radial structure of these
Jet Emitting Disks (JED) should then be compared to that of standard accretion
disks. The analytical treatment used in this work is very similar to that of
standard accretion disks but is using the parameter space of Magnetised
Accretion-Ejection Structures that include the jet torque on the underlying
disk. In this framework, the analytical expressions of key quantities, such as
mid-plane temperatures, surface densities or disk aspect ratio are derived. It
is found that JEDs present a structure very different from the SADs and that
can be observationally tested. The implications on planet formation in the
inner regions of accretion disks are briefly discussed. We also supply sets of
analytical formulae, valid in different opacity regimes, for the disk
quantities. These expressions can be readily used for any work where the disk
structure is needed as an input for the model.
