directions for particle flows are allowed. For $r>r_{lim}$ only outgoing current is possible. Figure 1 shows our 3D outer gap structure. Two pencil beams represent radio beams. The light budge grey shadow is the surface of last closed magnetic field lines, two dark surfaces represent the upper boundaries of two outer gaps. So the structure of the outer gap starts from the null surface and end at the light cylinder. The lower boundary is last closed field surface and the upper boudary is shown in Figure 1.

![image](f1_bw_300_1){width="75mm"}

[Fig. 1. 3D structure of the outer-magnetospheric gaps.\[fig:f1\]]{}

![image](f2){width="110mm"}

[Fig. 2. Emission projection onto the ($\zeta $, $\Phi $) plane and pulse profile. The emission consists of the emission outwards from both outer gaps and inwards only from the region ($r_{lim}-r_{in}$) of both outer gaps. The outer gaps are limited along the azimuthal direction by pair production. Crab parameters, $\alpha=65^\circ $, $\zeta =82^\circ $ and $\Delta \Phi =160^\circ $ are used.\[fig:f2\]]{}

EMISSION MORPHOLOGIES AND LIGHT CURVES
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In this section, we discuss the morphological features of emission from the three dimensional outer gaps. It is important to note that in order to properly describe the three-dimensional pulsar magnetosphere three-dimensional rotating dipolar magnetic 