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For dark matter (DM) particles with masses in the 0.6 - 6 m_p range, we setstringent constraints on the interaction cross-sections for scattering withordinary baryonic matter. These constraints follow from the recognition thatsuch particles can be captured by - and thermalized within - the Earth, leadingto a substantial accumulation and concentration of DM that interact withbaryons. Here, we discuss the probability that DM intercepted by the Earth willbe captured, the number of DM particles thereby accumulated over Earth'slifetime, the fraction of such particles retained in the face of evaporation,and the density distribution of such particles within the Earth. In the lattercontext, we note that a previous treatment of the density distribution of DM,presented by Gould and Raffelt and applied subsequently to DM in the Sun, isinconsistent with considerations of hydrostatic equilibrium. Our analysisprovides an estimate of the DM particle density at Earth's surface, which mayexceed 1.E+14 cm-3 for the mass range under consideration. Based upon ourdetermination of the DM density at Earth's surface, we derive constraints onthe scattering cross-sections. These constraints are placed by fourconsiderations: (1) the lifetime of the relativistic proton beam at the LargeHadron collider (LHC); (2) the orbital decay of spacecraft in low Earth orbit(LEO); (3) the vaporization rate of cryogenic liquids in well-insulated storagedewars; and (4) the thermal conductivity of Earth's crust. As an exampleapplication of our results, we show that for the scattering cross-sections thatwere invoked recently in Barkana's original explanation for the anomalouslydeep 21 cm absorption reported by EDGES, DM particle masses in the 0.6 - 4 m_prange are ruled out.

Dark Matter that Interacts with Baryons: Density Distribution within the Earth and New Constraints on the Interaction Cross-section