Weakly-Interacting Massive Particles in Non-supersymmetric SO(10) Grand Unified Models

Olive, Keith A.; Zheng, Jiaming

doi:10.48550/arxiv.1509.00809

Cited by 18 publications

(63 citation statements)

References 33 publications

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“…Also stable candidate of dark matter within the context of SO(10) GUT has been discussed in Refs. [59][60][61][62][63][64][65]. In the present left-right symmetric model, we have both left-handed as well as right-handed fermion triplet dark matter with a tiny mass splitting.…”

Section: Gauge Coupling Unificationmentioning

confidence: 89%

Common origin of 3.55 keV x-ray line and gauge coupling unification with left-right dark matter

2017

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We present a minimal left-right dark matter framework that can simultaneously explain the recently observed 3.55 keV X-ray line from several galaxy clusters and gauge coupling unification at high energy scale. Adopting a minimal dark matter strategy, we consider both left and right handed triplet fermionic dark matter candidates which are stable by virtue of a remnant Z 2 (−1) B−L symmetry arising after the spontaneous symmetry breaking of left-right gauge symmetry to that of the standard model. A scalar bitriplet field is incorporated whose first role is to allow radiative decay of right handed triplet dark matter into the left handed one and a photon with energy 3.55 keV. The other role this bitriplet field at TeV scale plays is to assist in achieving gauge coupling unification at a high energy scale within a non-supersymmetric SO(10) model while keeping the scale of left-right gauge symmetry around the TeV corner. Apart from solving the neutrino mass problem and giving verifiable new contributions to neutrinoless double beta decay and charged lepton flavour violation, the model with TeV scale gauge bosons can also give rise to interesting collider signatures like diboson excess, dilepton plus two jets excess reported recently in the large hadron collider data.

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Section: Gauge Coupling Unificationmentioning

confidence: 89%

Common origin of 3.55 keV x-ray line and gauge coupling unification with left-right dark matter

2017

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“…The same interaction which leads to reheating (σφ 2 b 2 ) also brings the inflaton into thermal equilibrium and the inflaton relic density is determined by standard freeze-out conditions. Inflaton dark matter in this respect closely resembles a scalar singlet (Higgs portal) dark matter model [32,36,[65][66][67][68][69][70][71][72][73][74]. To avoid the constraints from direct detection experiments [75][76][77], we must be in one of two mass regimes for m φ : either σ, is relatively large (of order 1) and the inflaton mass is in the range m φ ∼ 1 − 5 TeV (where the upper limit stems from the perturbativity of the couplings) or σ ∼ 10 −4 −4×10 −3 and m φ m h /2 = 62.6 GeV, and the relic density is determined by the resonant annihilation of the inflaton.…”

Section: Introductionmentioning

confidence: 90%

“…The case of an inflaton as dark matter is completely indistinguishable from the generic model called "scalar singlet Higgs portal" [32,36,[65][66][67][68][69][70][71][72][73] (for a review of models, see [74]). Indeed, the potential described in Eq.…”

Section: Dark Mattermentioning

confidence: 99%

On the Realization of WIMPflation

Garcia,

Mambrini,

Olive

et al. 2021

Preprint

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We consider models for inflation with a stable inflaton. Reheating is achieved through scattering processes such as φφ → hh, where h is the Standard Model Higgs boson. We consider the reheating process in detail and show that for a relatively large coupling (needed for the late annihilations of the inflaton during freeze-out), reheating is almost instantaneous leading to a relatively high reheating temperature. The process φφ ↔ hh brings the inflaton back into equilibrium, leading to a well studied scalar singlet dark matter candidate and Higgs portal model. We argue that such models can be derived from no-scale supergravity.

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“…2) The interaction of the dark matter particles with radiation bath could be too weak to attain thermal equilibrium before it freezes out. This mechanism is referred to as the freeze-in mechanism, and the produced dark matter particles are generally known as feebly interacting dark matter (FIMP) [17][18][19][20][21][22][23][24][25][26]. For gravitationally produced dark matter freeze-in mechanism will be effective, and dark matter produced from the radiation bath will have both possibilities of freeze-in and freeze-out production.…”

Section: B Reheating Parameters and Observable Constraintsmentioning

confidence: 99%

Gravitational dark matter: free streaming and phase space distribution

Haque¹,

Maity²

2021

Preprint

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Gravitational dark matter (DM) is the simplest possible scenario that has recently gained interest in the early universe cosmology. In this scenario, DM is assumed to be produced from the decaying inflaton through the gravitational interaction during reheating. Gravitational production from the radiation bath will be ignored as our analysis shows it to be suppressed for a wide range of reheating temperature (T re ).Ignoring any other internal parameters except the DM mass (m Y ) and spin, a particular inflation model such as α-attractor, with a specific scalar spectral index (n s ) has been shown to uniquely fix the dark matter mass of the present universe. For fermion type dark matter we found the mass m f should be within (10 4 − 10 13 ) GeV, and for boson type DM, the mass m s/X turned out to be within (10 −8 − 10 13 ) GeV.Interestingly, if the inflaton equation of state ω φ → 1/3, the DM mass also approaches towards unique value, m f ∼ 10 10 GeV and m s/X ∼ 10 3 ( 8 × 10 3 ) GeV irrespective of the value of ω φ . We further analyzed the phase space distribution (f Y ), and free streaming length (λ f s ) of these gravitationally produced DM. f Y , which is believed to encode important information about DM, is shown to contain a characteristic primary peak at the initial time where the gravitational production is maximum for both fermion/boson. Apart from this fermionic phase-space distribution function contains an additional peak near the inflaton and fermion mass equality (m Y = m φ ) arising for ω φ > 5/9. Furthermore, the height of this additional peak turned out to be increasing with decreasing T re , and at some point dominates over the primary one. Since reheating is a causal process and dark matter is produced during this phase, gravitational instability forming small-scale DM structures during this period will encode those phase space information and be observed at present. Crucial condition λ f s < λ re of forming such small scale DM structure during reheating has been analyzed in detail. We further estimate in detail the range of scales within which the above condition will be satisfied for different dark matter masses. Finally, we end by stating the fact that all our results are observed to be insensitive on the parameter α of the inflaton potential within the allowed range set by the latest Planck and BICEP/Keck results.

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Weakly-Interacting Massive Particles in Non-supersymmetric SO(10) Grand Unified Models

Cited by 18 publications

References 33 publications

Common origin of 3.55 keV x-ray line and gauge coupling unification with left-right dark matter

Common origin of 3.55 keV x-ray line and gauge coupling unification with left-right dark matter

On the Realization of WIMPflation

Gravitational dark matter: free streaming and phase space distribution

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