The inner annular Gap for pulsar radiation: gamma-ray and radio emission

The inner annular gap (IAG), a new type of inner gap whose magnetic field lines intersect the null charge surface (NCS), is proposed to explain $\gamma$-ray and radio emission from pulsars. The IAG can be an important source for high-energy particles. The particles can radiate between the NCS and the IAG. Some observational characteristics in both $\gamma$-ray and radio bands, such as the $\gamma$-ray emission beams of Crab-like, Vela-like and Geminga-like, can be reproduced by numerical method. It is predicted that the view angle $\zeta$ should be larger than the inclination angle ($\zeta>\alpha$), otherwise the $\gamma$-ray radiation will have little possibility to be observed. Whether the inner annular gap (or cap) is sparking (or free flow) depends on the surface binding energy of the pulsar. In stead of neutron star models, the scenario of the IAG is favorable for bare strange star models, because bare strange stars can easily satisfy the requisite condition to form an IAG for both pulsars ($\vec{\Omega}\cdot \vec{B}<0$) and anti-pulsars ($\vec\Omega \cdot \vec{B}>0$).