these dark matter models via observation of gamma rays and charged particles in the solar system.

2. Capture and delayed electromagnetic decays of mediators {#capture-and-delayed-electromagnetic-decays-of-mediators .unnumbered}
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In this section we derive the general formulae for the expected gamma ray fluxes generated by metastable mediator decays. We will also consider the case of charged particle fluxes and comment on the expected effect of the magnetic fields of the Sun and Earth.

### 2.1 Solar capture and $\gamma$-flux {#solar-capture-and-gamma-flux .unnumbered}

We begin by providing the trapping efficiency of WIMPs inside the Sun, assuming elastic scattering of WIMPs on nuclei [@Gould; @Kamionkowski; @review] and normalizing unknown quantities on some fiducial values: C\_ 1.3 10\^[21]{} [s]{}\^[-1]{} ( ) \_N f\_N () S(m\_/m\_N) F\_N(m\_), \[scaling\] where the sum runs over the nuclei $N$ present in the Sun, $f_N$ denotes the fractional abundance relative to hydrogen, $\sigma^{\rm SD}_N$ $(\sigma^{\rm SI}_N)$ is the spin-dependent(spin-independent) scattering cross section and we have used the standard values $\rho_\chi = 0.3$ GeV cm$^{-3}$ and $\bar{v} = 270$ km/s for the local WIMP density and velocity dispersion. The function $S(x)=[A(x)^{3/2}/(1+A(x)^{3/2}) ]^{2/3}$, where $A(x) = (3/2)[x/(x-1)^2](v_{esc}/{\bar v})^2$, with $v_{esc} \simeq 1156$ km/s an ‘effective’ escape velocity, is a kinematic suppression factor, while 