Compact dark matter objects via N dark sectors

Abstract

We propose a novel class of compact dark matter objects in theories where the dark matter consists of multiple sectors. We call these objects N -MACHOs. In such theories neither the existence of dark matter species nor their extremely weak coupling to the observable sector represent additional hypotheses but instead are imposed by the solution to the Hierarchy Problem and unitarity. The crucial point is that particles from the same sector have non-trivial interactions but interact only gravitationally otherwise. As a consequence, the pressure that counteracts the gravitational collapse is reduced while the gravitational force remains the same. This results in collapsed structures much lighter and smaller as compared to the ordinary single-sector case. We apply this phenomenon to a dark matter theory that consists of N dilute copies of the Standard Model. The solutions do not rely on an exotic stabilization mechanism, but rather use the same well-understood properties as known stellar structures. This framework also gives rise to new microscopic superheavy structures, for example with mass 10 8 g and size 10 −13 cm. By confronting the resulting objects with observational constraints, we find that, due to a huge suppression factor entering the mass spectrum, these objects evade the strongest constrained region of the parameter space. Finally, we discuss possible formation scenarios of N -MACHOs. We argue that, due to the efficient dissipation of energy on small scales, high-density regions such as ultra-compact mini-halos could serve as formation sites of N -MACHOs. * Electronic address: emi@mpp.mpg.de 1 An example of the theory that obeys such a standard is that of the axion [1,2], which is motivated by the Peccei-Quinn solu-arXiv:1911.13281v1 [astro-ph.CO]

Black Hole Metamorphosis and Stabilization by Memory Burden

“…Constraints would be similar to the ones on N-MACHOs[34] 8. We are not aware of an observational lower bound on the diffuse galactic gamma-ray flux at photon energies Eγ ∼ 10 5 GeV.…”

“…For the present values of the remaining parameters (34), such values are rare. In order to illustrate this point, we plot the maximal amplitude of oscillations as a function of C m in Fig.…”

Orbital Dynamics in the Restricted Three Body Problem: Overview of Recent Analytical Advances Obtained by Separating Rapid and Slow Subsystems in Non-Planar Configurations

“…Compact dark matter objects (CDOs) have been the subject of many discussions in the literature (for the latest publications, refer to the papers by Errehymy et al [44], Hadjimichef et al [45], Raidal et al [46], Dvali et al [47], Horowitz et al [48], Liao et al [49], and the references therein). The mass and the distance of the CDOs are usually estimated via the gravitational microlensing effect.…”

“…In the next step, one can use Equation (3) from Section 2 (for the scaled equilibrium radius v(w, b) of the planetary orbit) to find out the sole remaining unknown quantity b = M/m, while employing the definitions of w and v from Equation (47). Oks [33] demonstrated a method for analytically obtaining the unknown mass M of the CDO and its unknown distance R from the star by employing the following input parameters: z 0 , ρ 0 (the equilibrium radius of the planetary orbit), m (the star mass), and the orbital frequency F (or the orbital period T) of the planet.…”

“…In the next step, one can use Equation (3) from Section 2 (for the scaled equilibrium radius v(w, b) of the planetary orbit) to find out the sole remaining unknown quantity b = M/m, while employing the definitions of w and v from Equation (47).…”