Abstract
Quark nuggets are a candidate for dark matter consistent with the Standard Model. Previous models of quark nuggets have investigated properties arising from their being composed of strange, up, and down quarks and have not included any effects caused by their self-magnetic field. However, Tatsumi found that the core of a magnetar star may be a quark nugget in a ferromagnetic state with core magnetic field Bsurface = 1012±1 T. We apply Tatsumi’s result to quark-nugget dark-matter and report results on aggregation of magnetized quark nuggets (MQNs) after formation from the quark-gluon plasma until expansion of the universe freezes out the mass distribution to ~ 10−24 kg to ~ 1014 kg. Aggregation overcomes weak-interaction decay. Computed mass distributions show MQNs are consistent with requirements for dark matter and indicate that geologic detectors (craters in peat bogs) and space-based detectors (satellites measuring radio-frequency emissions after passage through normal matter) should be able to detect MQN dark matter. Null and positive observations narrow the range of a key parameter Bo ~ Bsurface to 1 × 1011 T < Bo ≤ 3 × 1012 T.
Highlights
Quark nuggets are a candidate for dark matter consistent with the Standard Model
Since magnetized quark nuggets (MQNs) are a ferromagnetic liquid in Tatsumi’s theory[16], the domains align after aggregation and the surface magnetic field is preserved, so Bo is preserved in aggregations
We have explored the consequences of his theory as applied to dark matter
Summary
Quark nuggets are a candidate for dark matter consistent with the Standard Model. Previous models of quark nuggets have investigated properties arising from their being composed of strange, up, and down quarks and have not included any effects caused by their self-magnetic field. Tatsumi[16] explored the internal state of quark-nugget cores in magnetars and found they may exist as a ferromagnetic liquid with a surface magnetic field Bsurface = 1012±1 T. His theory uses the bag model[21] because more rigorous lattice and perturbative calculations with chromodynamics are intractable for the relevant energy scale of ~ 90 MeV. Αc gets larger as the energy scale decreases, it is not known if αc is that large Even with those considerations, his conclusions have important consequences and are testable through searches for quark-nugget dark matter. If more accurate values of ρDM when T ~ 100 MeV, ρQN, or Bo are found, Eq (1) can give a correspondingly more accurate value of
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