Macro dark matter

Abstract

Dark matter is a vital component of the current best model of our universe, ΛCDM. There are leading candidates for what the dark matter could be (e.g. weaklyinteracting massive particles, or axions), but no compelling observational or experimental evidence exists to support these particular candidates, nor any beyond-the-Standard-Model physics that might produce such candidates. This suggests that other dark matter candidates, including ones that might arise in the Standard Model, should receive increased attention. Here we consider a general class of dark matter candidates with characteristic masses and interaction cross-sections characterized in units of grams and cm 2 , respectively -we therefore dub these macroscopic objects as Macros. Such dark matter candidates could potentially be assembled out of Standard Model particles (quarks and leptons) in the early universe. A combination of Earth-based, astrophysical, and cosmological observations constrain a portion of the Macro parameter space. A large region of parameter space remains, most notably for nuclear-dense objects with masses in the range 55 − 10 17 g and 2 × 10 20 − 4 × 10 24 g, although the lower mass window is closed for Macros that destabilize ordinary matter.

Solar Extreme UV radiation and quark nugget dark matter model

“…To reiterate the same claim: the allowed window for the baryon charge B (and corresponding radiation energy due to annihilation of the anti-nuggets) is perfectly consistent with all presently available constraints. 7 The smallest nuggets with B ∼ (10 23 − 10 24 ) naively contradict to the constraints cited in [46]. However, the corresponding constraints are actually derived with the assumption that nuggets with a definite mass (smaller than 55g) saturate the dark matter density.…”

“…[18,46] for review 7 . To reiterate the same claim: the allowed window for the baryon charge B (and corresponding radiation energy due to annihilation of the anti-nuggets) is perfectly consistent with all presently available constraints.…”

Terrestrial and martian heat flow limits on dark matter

“…On the other hand, near-surface direct detection experiments [8] are more sensitive to strongly-interacting DM, along with repurposed high-altitude detectors like the XQC rocket [9]. Constraints on strongly-interacting DM from these experiments are supplemented by numerous astrophysical bounds, including analyses of the cosmic microwave background [10,11], interstellar gas cooling [12,13], and a conspicuous lack of tracks in ancient mica [14][15][16]. This article will reinforce and extend existing constraints on DM's spin-independent interactions.…”

Compact bifluid hybrid stars: hadronic matter mixed with self-interacting fermionic asymmetric dark matter

“…Moreover, a dark star of comparable mass may as well accrete neutron star matter to form a dark matter dominated neutron star. In addition to axions and WIMPs, a general class of dark matter candidates, called Macros, have been suggested that would have macroscopic size and mass [20].…”