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The structure of accretion disks is a fundamental issue regarding star and planet formation. Many theoretical studies, focusing on different aspects, have been conducted in the context of the Standard Accretion Disk (SAD) model, where no jet is present. We aim at calculating the structure of YSO accretion disk in an approach that takes into account the presence of the protostellar jets. The radial structure of this Jet Emitting Disk (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 the Magnetised Accretion-Ejection Structures (MAES) to include the effects of the jet on the disk. In this framework, the analytical expressions of key quantities, such as mid-plane temperatures, surface densities or disk aspect ratio can be derived. It is found that JED are both thinner and lighter than SAD. The way this may affect planet formation and migration is briefly addressed.