Supersymmetric superheavy dark matter

Berezinsky, V.; Kachelrieß, M.; Solberg, M. Aa.

doi:10.1103/physrevd.78.123535

Cited by 31 publications

(44 citation statements)

References 56 publications

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“…Interestingly enough, the dark matter candidates, which are the lightest particles among W -particles carrying abnormal B − L numbers, are superheavy in the inflation regime, and this is called superheavy dark matter [25][26][27][28][29][30][31][32][33][34][35][36][37][38][39][40][41][42][43]. They are stabilized by W -parity as a residual gauge symmetry.…”

Section: Introductionmentioning

confidence: 99%

Neutrino masses and superheavy dark matter in the 3-3-1-1 model

Huong

Dong

2017

Eur. Phys. J. C

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In this work, we interpret the 3-3-1-1 model when the B − L and 3-3-1 breaking scales behave simultaneously as the inflation scale. This setup not only realizes the previously achieved consequences of inflation and leptogenesis, but also provides new insights in superheavy dark matter and neutrino masses. We argue that the 3-3-1-1 model can incorporate a scalar sextet, which induces both small masses for the neutrinos via a combined type I and II seesaw and large masses for the new neutral fermions. Additionally, all the new particles have large masses in the inflation scale. The lightest particle among the W -particles that have abnormal (i.e., wrong) B − L number in comparison to those of the standard model particles may be superheavy dark matter as it is stabilized by W -parity. The dark matter candidate may be a Majorana fermion, a neutral scalar, or a neutral gauge boson, which was properly created in the early universe due to gravitational effects on the vacuum or thermal production after cosmic inflation.

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Section: Introductionmentioning

confidence: 99%

Neutrino masses and superheavy dark matter in the 3-3-1-1 model

Huong

Dong

2017

Eur. Phys. J. C

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“…Model also possess superheavy dark matter candidates (see, e.g., [61][62][63][64][65][66][67][68][69][70][71]). Since there are many scalar field degrees of freedom in typical BSMs, the possibility of identifying one of these scalars with σ is also plausible.…”

Section: Fermion Isocurvature Modelmentioning

confidence: 99%

Fermionic isocurvature perturbations

2015

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Isocurvature perturbations in the inflationary literature typically involve quantum fluctuations of bosonic field degrees of freedom. In this work, we consider isocurvature perturbations from fermionic quantum fluctuations during inflation. When a stable massive fermion is coupled to a non-conformal sector different from the scalar metric perturbations, observably large amplitude scale invariant isocurvature perturbations can be generated. In addition to the computation of the isocurvature two-point function, an estimate of the local non-Gaussianities is also given and found to be promising for observations in a corner of the parameter space. The results provide a new class of cosmological probes for theories with stable massive fermions. On the technical side, we explicitly renormalize the composite operator in curved spacetime and show that gravitational Ward identities play an important role in suppressing certain contributions to the fermionic isocurvature perturbations.

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“…For the squared Feynman amplitude leading to the expression (2.5) for the energy relaxation time, confer [1].…”

Section: Pos(idm2008)092mentioning

confidence: 99%

“…The other channels are of order O(m 4 Z /M 4 SUSY ) (or less), see [1] for exact expressions. With |M χ 0 χ 0 →χ 0 χ 0 | 2 = |M h-exch | 2 , the total cross section of neutralino-neutralino scattering follows as…”

Section: Elastic Neutralino-neutralino Scatteringmentioning

confidence: 99%

“…Annihilations of superheavy neutralinos are, in the bino case, dominated by the channels Z + H, h + A, A + H, W ± + H ∓ , since all other channels are suppressed by powers of m Z /M SUSY . In the higgsino case all bosonic channels contribute at leading order except annihilation into Z 0 + A 0 and h + H. See [1] for the squared matrix elements of the dominating channels.…”

Section: Annihilationsmentioning

confidence: 99%

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Superheavy neutralinos as dark matter particles

Berezinsky¹,

Kachelrieß²,

Solberg³

2009

Proceedings of Identification of Dark Matter 2008 — PoS(idm2008)

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We propose the lightest supersymmetric particle (LSP) as a well-suited candidate for superheavy dark matter. The mass m χ of the LSP should be above 3 × 10 11 GeV, so that gravitational interactions at the end of inflation can produce it with the correct abundance, Ω χ h 2 ∼ 0.1. Weak interactions remain perturbative despite the large mass hierarchy, m χ m Z , because of the special decoupling properties of supersymmetry. As a result the model is predictive and we discuss elastic scattering of neutralinos on light fermions, self-scatterings and briefly annihilations within this scheme. Identification of dark matter

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Supersymmetric superheavy dark matter

Cited by 31 publications

References 56 publications

Neutrino masses and superheavy dark matter in the 3-3-1-1 model

Neutrino masses and superheavy dark matter in the 3-3-1-1 model

Fermionic isocurvature perturbations

Superheavy neutralinos as dark matter particles

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