Maximally self-interacting dark matter: models and predictions

Kamada, Ayuki; Kim, Hee Jung; Kuwahara, Takumi

doi:10.1007/jhep12(2020)202

“…15 There are also arguments in favor of finite interaction cross sections from the the dwarf irregular galaxies [72], the low surface brightness galaxies [73], and galaxy clusters [74] (see also refs. [75][76][77]).…”

Section: Jhep07(2021)220mentioning

confidence: 99%

Chiral composite asymmetric dark matter

Ibe

¹

,

Kobayashi

²

,

Watanabe

³

2021

J. High Energ. Phys.

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The asymmetric dark matter (ADM) scenario solves the baryon-dark matter coincidence problem when the dark matter (DM) mass is of $$ \mathcal{O}(1) $$ O 1 GeV. Composite ADM models based on QCD-like strong dynamics are particularly motivated since the strong dynamics naturally provides the DM mass of $$ \mathcal{O}(1) $$ O 1 GeV and the large annihilation cross-section simultaneously. In those models, the sub-GeV dark photon often plays an essential role in transferring the excessive entropy in the dark sector into the visible sector, i.e., the Standard Model sector. This paper constructs a chiral composite ADM model where the U(1)D gauge symmetry is embedded into the chiral flavor symmetry. Due to the dynamical breaking of the chiral flavor symmetry, the model naturally provides the masses of the dark photon and the dark pions in the sub-GeV range, both of which play crucial roles for a successful ADM model.

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“…In particular, the latter can be computed by integrating eq. (C.1) over the velocity distribution function, obtaining the average rate for particles at position r [50] Γ scatt ( r) = σ v pair ( r) ρ( r) m χ , (C. 19) where ρ( r) is given by eq. (C.17) and σ v pair = σ v pair if the scattering cross section is velocity-independent.…”

Section: Jhep04(2021)223mentioning

confidence: 99%

“…For instance, the annihilation rate extracted from simulations can be compared to the analytic result, which is given by eq. (C. 19) with the replacement of σ v pair with σ ann v . The extracted annihilation rate as a function of the radius r has been obtained in the same way as done for scattering events, namely as the ratio between the number of annihilated particles located in the radial bin including r and the time averaged number of particles within the same bin.…”

Section: Jhep04(2021)223mentioning

confidence: 99%

“…Like other exothermic processes, this has the advantage of predicting a cross section with σv remaining constant at low velocities, as desired for fitting the DM profiles of both large and small galactic structures. Other interesting possibilities to achieve the correct velocity-dependence of SIDM have been studied, for instance in the context of resonant SIDM [11][12][13], puffy DM [14], self-heating DM [15][16][17][18], maximally SIDM [19] and DM bound states produced in the early universe by three-body recombination [20,21].…”

Section: Introductionmentioning

confidence: 99%

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Late-time dark matter oscillations and the core-cusp problem

Cline

¹

,

Gambini

²

,

McDermott

³

et al. 2021

J. High Energ. Phys.

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The core-cusp problem persists as an unresolved tension between the pre- dictions of ΛCDM cosmology and observations of dark matter (DM) profiles in dwarf spheroidal and other galaxies. We present a novel scenario for converting cusps into cores through reactivation of DM annihilation in galaxies at late times. This can happen in asymmetric DM models when there is a very small DM-number violating mass term that causes oscillations between DM and its antiparticle. Using analytic methods as well as gravitational N-body simulations, we show that this mechanism can robustly eliminate cusps from galactic DM profiles for light fermionic DM of mass mχ ∼ (0.1 − 1) GeV and a lighter mediator into which the DM can annihilate. We identify regions of parameter space where annihilation of DM particles is more efficient than elastic scattering at reducing the inner density of the DM profile. Dark matter annihilation is therefore a qualitatively distinct alternative to the mechanism of elastic self-interacting dark matter for addressing the cusp-core problem.

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“…Among these, the gauged U (1) L μ −L τ stands out for its simplicity, as it is anomaly free without the addition of any extra new fermion fields [29][30][31]. Various realisations of this model have been studied, including also additional neutrino [31][32][33] and dark matter (DM) fields [34][35][36][37]. Recently, it has also been noted that a simultaneous explanation of the Hubble tension can be achieved in these models [38,39].…”

Section: Introductionmentioning

confidence: 99%

Confirming $$U(1)_{L_\mu -L_{\tau }}$$ as a solution for $$(g-2)_\mu $$ with neutrinos

Amaral

¹

,

Cerdeño

²

,

Cheek

³

et al. 2021

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The recent measurement of the muon anomalous magnetic moment by the Fermilab E989 experiment, when combined with the previous result at BNL, has confirmed the tension with the SM prediction at $$4.2\,\sigma $$ 4.2 σ CL, strengthening the motivation for new physics in the leptonic sector. Among the different particle physics models that could account for such an excess, a gauged $$U(1)_{L_\mu -L_{\tau }}$$ U ( 1 ) L μ - L τ stands out for its simplicity. In this article, we explore how the combination of data from different future probes can help identify the nature of the new physics behind the muon anomalous magnetic moment. In particular, we contrast $$U(1)_{L_\mu -L_{\tau }}$$ U ( 1 ) L μ - L τ with an effective $$U(1)_{L_\mu }$$ U ( 1 ) L μ -type model. We first show that muon fixed target experiments (such as NA64$$\mu $$ μ ) will be able to measure the coupling of the hidden photon to the muon sector in the region compatible with $$(g-2)_\mu $$ ( g - 2 ) μ , and will have some sensitivity to the hidden photon’s mass. We then study how experiments looking for coherent elastic neutrino-nucleus scattering (CE$$\nu $$ ν NS) at spallation sources will provide crucial additional information on the kinetic mixing of the hidden photon. When combined with NA64$$\mu $$ μ results, the exclusion limits (or reconstructed regions) of future CE$$\nu $$ ν NS detectors will also allow for a better measurement of the mediator mass. Finally, the observation of nuclear recoils from solar neutrinos in dark matter direct detection experiments will provide unique information about the coupling of the hidden photon to the tau sector. The signal expected for $$U(1)_{L_\mu -L_{\tau }}$$ U ( 1 ) L μ - L τ is larger than for $$U(1)_{L_\mu }$$ U ( 1 ) L μ with the same kinetic mixing, and future multi-ton liquid xenon proposals (such as DARWIN) have the potential to confirm the former over the latter. We determine the necessary exposure and energy threshold for a potential $$5\,\sigma $$ 5 σ discovery of a $$U(1)_{L_\mu -L_{\tau }}$$ U ( 1 ) L μ - L τ boson, and we conclude that the future DARWIN observatory will be able to carry out this measurement if the experimental threshold is lowered to $$1\,{\mathrm {keV}}_{\mathrm {nr}} $$ 1 keV nr .

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Maximally self-interacting dark matter: models and predictions

Cited by 29 publications

References 175 publications

Chiral composite asymmetric dark matter

Chiral composite asymmetric dark matter

Late-time dark matter oscillations and the core-cusp problem

Confirming $$U(1)_{L_\mu -L_{\tau }}$$ as a solution for $$(g-2)_\mu $$ with neutrinos

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