the fully differential flux $\frac{{\textrm{d}}^2\Phi(p, \theta)}{{\textrm{d}}p\,{\textrm{d}}\Omega}/
(C_\odot \textrm{Br}_V \textrm{Br}_\gamma
m_\chi^{-1} \cdot 10^{-21}\textrm{cm}^{-2})$ in the direction $\theta=0$, averaged over a Gaussian profile that mimics an angular resolution of $\Delta\theta=0.1 \theta_\odot$; (c) The same for $\theta = 0.1 \theta\odot$.]{} ](signal){width="100.00000%"}

Up to this point we have only discussed the spectrum of photons resulting from the decays of long-lived mediators. A similar analysis for charged particles, such as electrons and positrons, is less straightforward due to the complications of the magnetic fields of the Sun and Earth, as well as the solar wind, and their effects on the propagation, energy degradation, and absorption. A proper calculation of the angular and energy distributions is beyond the scope of this work, but we wish to give a qualitative discussion of these effects, paying particular attention to the implications regarding a possible local solar system component to the PAMELA signal.

A variety of secluded models may be constructed which can lead to electrons and positrons in the final state. It is important to stress that the effects of the magnetic fields and solar atmosphere on these charged states is quite model dependent, and primarily sensitive to the lifetime and boost of the mediator produced in the 