scholarly journals Lepton-flavored asymmetric dark matter and interference in direct detection

2015 ◽  
Vol 91 (3) ◽  
Author(s):  
Ali Hamze ◽  
Can Kilic ◽  
Jason Koeller ◽  
Cynthia Trendafilova ◽  
Jiang-Hao Yu
Keyword(s):  
Dark Matter ◽  
Direct Detection ◽  
Asymmetric Dark Matter

scholarly journals Asymmetric dark matter: residual annihilations and self-interactions

2018 ◽  
Vol 4 (6) ◽  
Author(s):  
Iason Baldes ◽  
Marco Cirelli ◽  
Paolo Panci ◽  
Kalliopi Petraki ◽  
Filippo Sala ◽  
...  
Keyword(s):  
Dark Matter ◽  
Direct Detection ◽  
Galactic Structure ◽  
The Common ◽  
Asymmetric Dark Matter

Dark matter (DM) coupled to light mediators has been invoked to resolve the putative discrepancies between collisionless cold DM and galactic structure observations. However, \gammaγ-ray searches and the CMB strongly constrain such scenarios. To ease the tension, we consider asymmetric DM. We show that, contrary to the common lore, detectable annihilations occur even for large asymmetries, and derive bounds from the CMB, \gammaγ-ray, neutrino and antiproton searches. We then identify the viable space for self-interacting DM. Direct detection does not exclude this scenario, but provides a way to test it.

scholarly journals GeV SCALE ASYMMETRIC DARK MATTER FROM MIRROR UNIVERSE: DIRECT DETECTION AND LHC SIGNATURES

2012 ◽  
Vol 10 ◽  
pp. 21-34 ◽  
Author(s):  
JIAN-WEI CUI ◽  
HONG-JIAN HE ◽  
LAN-CHUN LÜ ◽  
FU-RONG YIN
Keyword(s):  
Dark Matter ◽  
Parity Violation ◽  
Direct Detection ◽  
Weak Interactions ◽  
Dark Matter Particle ◽  
Interaction Terms ◽  
Parity Symmetry ◽  
The Common ◽  
Asymmetric Dark Matter ◽  
The Right

Mirror universe is a fundamental way to restore parity symmetry in weak interactions. It naturally provides the lightest mirror nucleon as a unique GeV-scale asymmetric dark matter particle candidate. We conjecture that the mirror parity is respected by the fundamental interaction Lagrangian, and its possible soft breaking arises only from non-interaction terms in the gauge-singlet sector. We realize the spontaneous mirror parity violation by minimizing the vacuum Higgs potential, and derive the corresponding Higgs spectrum. We demonstrate that the common origin of CP violation in the visible and mirror neutrino seesaws can generate the right amount of matter and mirror dark matter via leptogenesis. We analyze the direct detections of GeV-scale mirror dark matter by TEXONO and CDEX experiments. We further study the predicted distinctive Higgs signatures at the LHC.

scholarly journals REVIEW OF ASYMMETRIC DARK MATTER

2013 ◽  
Vol 28 (19) ◽  
pp. 1330028 ◽  
Author(s):  
KALLIOPI PETRAKI ◽  
RAYMOND R. VOLKAS
Keyword(s):  
Dark Matter ◽  
Direct Detection ◽  
Visible Matter ◽  
Asymmetric Dark Matter

Asymmetric dark matter models are based on the hypothesis that the present-day abundance of dark matter has the same origin as the abundance of ordinary or "visible" matter: an asymmetry in the number densities of particles and antiparticles. They are largely motivated by the observed similarity in the mass densities of dark and visible matter, with the former observed to be about five times the latter. This review discusses the construction of asymmetric dark matter models, summarizes cosmological and astrophysical bounds, and touches on direct detection prospects and collider signatures.

scholarly journals Direct detection of bound states of asymmetric dark matter

2019 ◽  
Vol 100 (3) ◽  
Author(s):  
Ahmet Coskuner ◽  
Dorota M. Grabowska ◽  
Simon Knapen ◽  
Kathryn M. Zurek
Keyword(s):  
Dark Matter ◽  
Bound States ◽  
Direct Detection ◽  
Asymmetric Dark Matter

scholarly journals WIMP cogenesis for asymmetric dark matter and the baryon asymmetry

2020 ◽  
Vol 2020 (12) ◽  
Author(s):  
Yanou Cui ◽  
Michael Shamma
Keyword(s):  
Dark Matter ◽  
Direct Detection ◽  
Massive Particle ◽  
Decay Chain ◽  
Baryon Number ◽  
High Energy ◽  
Baryon Asymmetry ◽  
Unified Framework ◽  
Low Mass ◽  
Asymmetric Dark Matter

Abstract We propose a new mechanism where asymmetric dark matter (ADM) and the baryon asymmetry are both generated in the same decay chain of a metastable weakly interacting massive particle (WIMP) after its thermal freezeout. Dark matter and baryons are connected by a generalized baryon number that is conserved, while the DM asymmetry and baryon asymmetry compensate each other. This unified framework addresses the DM-baryon coincidence while inheriting the merit of the conventional WIMP miracle in predicting relic abundances of matter. Examples of renormalizable models realizing this scenario are presented. These models generically predict ADM with sub-GeV to GeV-scale mass that interacts with Standard Model quarks or leptons, thus rendering potential signatures at direct detection experiments sensitive to low mass DM. Other interesting phenomenological predictions are also discussed, including: LHC signatures of new intermediate particles with color or electroweak charge and DM induced nucleon decay; the long-lived WIMP may be within reach of future high energy collider experiments.

scholarly journals Maximally self-interacting dark matter: models and predictions

2020 ◽  
Vol 2020 (12) ◽  
Author(s):  
Ayuki Kamada ◽  
Hee Jung Kim ◽  
Takumi Kuwahara
Keyword(s):  
Dark Matter ◽  
Cross Sections ◽  
Direct Detection ◽  
Model Parameters ◽  
Dwarf Spheroidal Galaxies ◽  
Unitarity Bound ◽  
Scattering Cross ◽  
Dark Matter Mass ◽  
Wide Range ◽  
Asymmetric Dark Matter

Abstract We study self-interacting dark matter (SIDM) scenarios, where the s-wave self-scattering cross section almost saturates the Unitarity bound. Such self-scattering cross sections are singly parameterized by the dark matter mass, and are featured by strong velocity dependence in a wide range of velocities. They may be indicated by observations of dark matter halos in a wide range of masses, from Milky Way’s dwarf spheroidal galaxies to galaxy clusters. We pin down the model parameters that saturates the Unitarity bound in well-motivated SIDM models: the gauged Lμ− Lτ model and composite asymmetric dark matter model. We discuss implications and predictions of such model parameters for cosmology like the H0 tension and dark-matter direct-detection experiments, and particle phenomenology like the beam-dump experiments.

scholarly journals The impact of inelastic self-interacting dark matter on the dark matter structure of a Milky Way halo

2020 ◽  
Author(s):  
Kun Ting Eddie Chua ◽  
Karia Dibert ◽  
Mark Vogelsberger ◽  
Jesús Zavala
Keyword(s):  
Dark Matter ◽  
High Speed ◽  
Cold Dark Matter ◽  
Milky Way ◽  
Direct Detection ◽  
Major Axis ◽  
Inelastic Collisions ◽  
Axis Ratio ◽  
Lower Velocity ◽  
The Impact

Abstract We study the effects of inelastic dark matter self-interactions on the internal structure of a simulated Milky Way (MW)-size halo. Self-interacting dark matter (SIDM) is an alternative to collisionless cold dark matter (CDM) which offers a unique solution to the problems encountered with CDM on sub-galactic scales. Although previous SIDM simulations have mainly considered elastic collisions, theoretical considerations motivate the existence of multi-state dark matter where transitions from the excited to the ground state are exothermic. In this work, we consider a self-interacting, two-state dark matter model with inelastic collisions, implemented in the Arepo code. We find that energy injection from inelastic self-interactions reduces the central density of the MW halo in a shorter timescale relative to the elastic scale, resulting in a larger core size. Inelastic collisions also isotropize the orbits, resulting in an overall lower velocity anisotropy for the inelastic MW halo. In the inner halo, the inelastic SIDM case (minor-to-major axis ratio s ≡ c/a ≈ 0.65) is more spherical than the CDM (s ≈ 0.4), but less spherical than the elastic SIDM case (s ≈ 0.75). The speed distribution f(v) of dark matter particles at the location of the Sun in the inelastic SIDM model shows a significant departure from the CDM model, with f(v) falling more steeply at high speeds. In addition, the velocity kicks imparted during inelastic collisions produce unbound high-speed particles with velocities up to 500 km s−1 throughout the halo. This implies that inelastic SIDM can potentially leave distinct signatures in direct detection experiments, relative to elastic SIDM and CDM.

scholarly journals Generalized blind spots for dark matter direct detection in the 2HDM

2020 ◽  
Vol 2020 (2) ◽  
Author(s):  
M. E. Cabrera ◽  
J. A. Casas ◽  
A. Delgado ◽  
S. Robles
Keyword(s):  
Dark Matter ◽  
Direct Detection ◽  
Blind Spots

scholarly journals Sensitivity of direct detection experiments to neutrino magnetic dipole moments

2020 ◽  
Vol 2020 (12) ◽  
Author(s):  
D. Aristizabal Sierra ◽  
R. Branada ◽  
O. G. Miranda ◽  
G. Sanchez Garcia
Keyword(s):  
Dark Matter ◽  
Magnetic Dipole ◽  
Direct Detection ◽  
Dipole Moments ◽  
Nuclear Recoil ◽  
Active Volume ◽  
Electron Recoil ◽  
Flux Measurements ◽  
Neutrino Fluxes ◽  
One Year

Abstract With large active volume sizes dark matter direct detection experiments are sensitive to solar neutrino fluxes. Nuclear recoil signals are induced by 8B neutrinos, while electron recoils are mainly generated by the pp flux. Measurements of both processes offer an opportunity to test neutrino properties at low thresholds with fairly low backgrounds. In this paper we study the sensitivity of these experiments to neutrino magnetic dipole moments assuming 1, 10 and 40 tonne active volumes (representative of XENON1T, XENONnT and DARWIN), 0.3 keV and 1 keV thresholds. We show that with nuclear recoil measurements alone a 40 tonne detector could be as competitive as Borexino, TEXONO and GEMMA, with sensitivities of order 8.0 × 10−11μB at the 90% CL after one year of data taking. Electron recoil measurements will increase sensitivities way below these values allowing to test regions not excluded by astrophysical arguments. Using electron recoil data and depending on performance, the same detector will be able to explore values down to 4.0 × 10−12μB at the 90% CL in one year of data taking. By assuming a 200-tonne liquid xenon detector operating during 10 years, we conclude that sensitivities in this type of detectors will be of order 10−12μB. Reducing statistical uncertainties may enable improving sensitivities below these values.

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