The Sun’s Dark Core: Helioseismic and Neutrino Flux Constraints on a Compact Solar Center

Abstract As dark matter appears to comprise most of the Galactic mass, some of it may accumulate in the cores of stars, thereby making the Sun a laboratory for constraining various dark matter theories. We consider the effects on the solar structure arising from a general class of macroscopic dark matter candidates that include strange quark matter, compact dark objects, and others. We calibrate standard solar evolution models (i.e., models that reproduce the mass, luminosity, radius, and metallicity of the Sun at its present age) with variable compact dark core masses ranging from 10 −8 to 10 −2 M ⊙ and assess their properties. We find that the weakest constraints come from solar neutrino flux measurements, which only rule out the most massive dark core comprising at least ∼1% of the total solar mass. The Sun’s acoustic oscillations impose stronger constraints, probing masses down to ∼10 −5 M ⊙ . We find that a model with a 10 −3 M ⊙ dark core appears to improve the agreement with helioseismic observations. We nevertheless caution against interpreting this as evidence for dark matter in the solar interior, and suggest plausible effects that the dark core may instead be emulating. Finally, we show that future measurements of solar g- modes may constrain dark core masses down to 10 −7 M ⊙ .