Type II seesaw and the PAMELA/ATIC signals

Gogoladze, Ilia; Okada, Nobuchika; Shafi, Qaisar

doi:10.1016/j.physletb.2009.07.035

Cited by 27 publications

(24 citation statements)

References 92 publications

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“…Interestingly, this extension essentially coincides with a model proposed in [23], and it can also account for the anomalous cosmic-ray positron flux reported by the PAMELA satellite experiment [24]. In addition, as analyzed in detail in [25], in the type-II seesaw extension of the SM, the vacuum stability bound on the Higgs boson mass can be reduced to coincide with the current experimental lower bound of 114.4 GeV [26].…”

supporting

confidence: 84%

WIMP dark matter inflation with observable gravity waves

Okada¹,

Shafi²

2011

Phys. Rev. D

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We present a successful inflation model based on λφ 4 potential in which a Standard Model (SM) singlet inflaton φ, with mass of around a TeV or less, also plays the role of a weakly interacting scalar dark matter particle (WIMP). The WIMP relic abundance generated after inflation is in accord with the current observations. The spectral index ns lies within the WMAP 1-σ bounds, while the Planck satellite may observe the tensorto-scalar ratio, a canonical measure of gravity waves, which we estimate lies between 0.003 and 0.007. An unbroken Z2 parity ensures that the scalar WIMP is absolutely stable.

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supporting

confidence: 84%

WIMP dark matter inflation with observable gravity waves

Okada¹,

Shafi²

2011

Phys. Rev. D

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“…The minimal type-II seesaw model can be extended to accommodate a cold DM candidate by simply adding a SM singlet real scalar field D [42]. Its stability can be ensured by assigning it an odd Z 2 parity, whereas all other fields are even under the Z 2 symmetry.…”

Section: Dark Mattermentioning

confidence: 99%

“…To understand the tiny neutrino masses, an isospin triplet scalar is added to the SM, which is automatically leptophilic in the sense that all the neutral, singly, and doubly charged components of the triplet decays predominantly into the SM leptons in a large parameter space. A scalar DM D is introduced to the minimal type-II seesaw model, which is stabilized by a discrete Z 2 symmetry [42,43]. Then an economical explanation of the e þ e − excess at 1.4 TeV could be the annihilation of DM with a mass ∼3 TeV into the doubly charged scalars which decays further into e AE e AE pairs, i.e., DD → H þþ H −− → e þ e þ e − e − .…”

Section: Introductionmentioning

confidence: 99%

Prospects of type-II seesaw models at future colliders in light of the DAMPEe+e−excess

Sui¹

2018

Phys. Rev. D

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The DAMPE e þ e − excess at around 1.4 TeV could be explained in the type-II seesaw model with a scalar dark mater D which is stabilized by a discrete Z 2 symmetry. The simplest scenario is the annihilation DD → H þþ H −− followed by the subsequent decay H AEAE → e AE e AE , with both the DM and triplet scalars roughly 3 TeV with a small mass splitting. In addition to the Drell-Yan process at future 100 TeV hadron colliders, the doubly charged components could also be produced at lepton colliders like ILC and CLIC in the off shell mode and mediate lepton flavor violating processes e þ e − → l AE i l ∓ j (with i ≠ j). A wide range of parameter space of the type-II seesaw could be probed, which are well below the current stringent lepton flavor constraints.

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“…A similar supersymmetric version of this mechanism where the neutralinos in the MSSM can annihilate to a scalar particle, which can then decay the observed excess in the cosmic ray data [125]. Models involving Type II see-saw mechanism [126] have also been considered recently where neutrino mass generation is linked with the positron excess. In addition to the above, it has been shown that extra dimensional models with KK gravitions can also produce the excess [127,127a].…”

Section: The Interpretationsmentioning

confidence: 99%

Results from PAMELA, ATIC and FERMI: Pulsars or dark matter?

2011

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It is well known that dark matter dominates the dynamics of galaxies and clusters of galaxies. Its constituents remain a mystery despite an assiduous search for them over the past three decades. Recent results from the satellite-based PAMELA experiment show an excess in the positron fraction at energies between 10 and 100 GeV in the secondary cosmic ray spectrum. Other experiments, namely ATIC, HESS and FERMI, show an excess in the total electron (e + + e − ) spectrum for energies greater than 100 GeV. These excesses in the positron fraction as well as the electron spectrum can arise in local astrophysical processes like pulsars, or can be attributed to the annihilation of the dark matter particles. The latter possibility gives clues to the possible candidates for the dark matter in galaxies and other astrophysical systems. In this article, we give a report of these exciting developments.

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Type II seesaw and the PAMELA/ATIC signals

Cited by 27 publications

References 92 publications

WIMP dark matter inflation with observable gravity waves

WIMP dark matter inflation with observable gravity waves

Prospects of type-II seesaw models at future colliders in light of the DAMPEe+e−excess

Results from PAMELA, ATIC and FERMI: Pulsars or dark matter?

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