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The energy released from dark matter annihilation leads to additionalionization and heating of the intergalactic gas and thereby impact the hydrogen21-cm signal during the cosmic dawn. The dark matter annihilation rate scalesas density-squared and it becomes inhomogeneously boosted along with structureformation. This paper examines the inhomogeneity in DM annihilation rateinduced by the growth of DM halo structures, and we show that this effect cansignificantly enhance the spatial fluctuations in gas temperature, gasionization fraction and consequently the 21-cm brightness temperature. Comparedto previous homogeneous calculations, inhomogeneous dark matter annihilationcan enhance the 21-cm power spectrum by orders of magnitude across the scalesof $k \in [0.05, 3]\ {\rm{Mpc^{-1}}}$. For a DM annihilation rate of$\left<\sigma v\right>/m_\chi \sim 10^{-27} {\rm cm^3 s^{-1} GeV^{-1}}$, thecorresponding signatures in the 21-cm power spectrum signal can be detected byupcoming radio observatories such as the SKA.

Signatures of inhomogeneous dark matter annihilation on 21-cm