Solar oscillations constrain a compact dark matter core in the Sun to below one hundred-thousandth of a solar mass, and a one-thousandth-solar-mass core improves helioseismic agreement by mimicking a heavy metal core.
Orbital motion of primordial black holes crossing Solar-type stars
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abstract
Primordial black holes (PBHs) are hypothetical objects that could have originated from density fluctuations in a very early phase of our Universe. Recent observations restrict the masses that such PBHs could have, if they are to constitute all of dark matter today: $10^{17} \, {\rm g} \leq m \leq 10^{23} \, {\rm g}$. With such low masses, general relativity predicts that the corresponding radii for the PBHs would be atomic or subatomic in size. When captured by a star, such a tiny PBH could exhibit an orbit completely or partially inside the body of the star, without significantly changing its mass for quite a long time. Here we examine the possible trajectories of a PBH that is captured by a Sun-like star. When in motion in the interior of the star, the amount of stellar mass that effectively interacts with the PBH will be a function of its distance to the center of the star. As a consequence, a strong effect on the shape of the orbits emerges, leading to PBH trajectories that could be open or closed, and exhibiting a rich variety of patterns.
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The Sun's Dark Core: Helioseismic and neutrino flux constraints on a compact solar center
Solar oscillations constrain a compact dark matter core in the Sun to below one hundred-thousandth of a solar mass, and a one-thousandth-solar-mass core improves helioseismic agreement by mimicking a heavy metal core.