Antiprotons from primordial black holes

Barrau, A.; Boudoul, G.; Donato, Fiorenza; Maurin, D.; Salati, Pierre; Taillet, R.

doi:10.1051/0004-6361:20020313

Cited by 85 publications

(133 citation statements)

References 53 publications

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“…Furthermore, we impose the free escape boundary condition, namely the positron density drops to zero on the surface of the diffusion zone. This means that the positrons coming from the outside of the zone are negligible, while the positrons produced inside the zone contribute to the flux around the solar system due to the trapping by the tangled magnetic field [31]. The diffusion zone is usually assumed to be a cylinder with the half-height (L) and radius (R), which are set to be L = 4 kpc and R = 20 kpc in this paper.…”

Section: Positron Propagation In Galaxymentioning

confidence: 99%

Cosmic positron signature from dark matter in the littlest Higgs model withTparity

et al. 2007

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We calculate the flux of cosmic positrons from the dark matter annihilation in the littlest Higgs model with T-parity. The dark matter annihilates mainly into weak gauge bosons in the halo, and high energy positrons are produced through leptonic and hadronic decays of the bosons. We investigate a possibility to detect the positron signal in upcoming experiments such as PAMELA and AMS-02. We found that the dark matter signal can be distinguished from the background in the PAMELA experiment when the dark matter mass is less than 120 GeV and the signal flux is enhanced due to a small scale clustering of dark matter. Furthermore, the signal from the dark matter annihilation can be detected in the AMS-02 experiment, even if such enhancement does not exist. We also discuss the invisible width of the Higgs boson in this model. 1 E-mail: masano@post.kek.jp 2 E-mail: smatsu@post.kek.jp 3 E-mail: okadan@post.kek.jp 4 E-mail: yasuhiro.okada@kek.jp I IntroductionThe hierarchy problem in the Standard Model (SM) is expected to give a clue to explore the physics beyond the SM. This problem is essentially related to quadratically divergent corrections to the Higgs boson mass, and we need a mechanism to avoid the divergences. To solve the problem, many scenarios have been proposed so far, for example supersymmetry, in which the divergences are completely removed.Other examples are scenarios with a low energy cutoff scale around a TeV such as Techni-color and TeV scale extra-dimension.The latter scenarios are, however, constrained by the electroweak precision measurements. From the analysis of higher dimensional operators at the cutoff scale, it has been found that the scale should be larger than roughly 5 TeV [1]. For such high energy cutoff, the hierarchy problem appears again: We still need the fine-tuning of a few percent level in the Higgs mass term in order to obtain the 100-200 GeV Higgs boson mass. This problem is called the little hierarchy problem.Recently the little Higgs model [2,3] has been proposed for solving the little hierarchy problem. In this scenario, the Higgs boson is regarded as a pseudo NambuGoldstone boson. New particles such as heavy gauge bosons and a top-partner are introduced, and all quadratic divergences to the Higgs mass term completely vanish at one-loop level due to these particles' contributions. Thus, the fine-tuning of the Higgs boson mass is avoided even if the cutoff scale is around 10 TeV.The original little Higgs model is still strongly constrained by the electroweak precision measurements [4]. This is mainly due to the contributions to electroweak observables from new heavy gauge bosons, because their masses are much smaller than the cutoff scale. In particular, direct couplings among a new heavy gauge boson and SM particles give sizable contributions to the observables. As a result, masses of new particles have to be raised, and the fine-tuning of the Higgs boson mass is reintroduced.To resolve the problem, the implementation of the Z 2 symmetry called T-parity to the model has b...

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Section: Positron Propagation In Galaxymentioning

confidence: 99%

Cosmic positron signature from dark matter in the littlest Higgs model withTparity

et al. 2007

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“…There are at least three models of exotic sources able to produce high-energy antiprotons: primordial black hole (PBH) evaporation [17], dark-matter neutralino annihilation [18,19] and high-energy antiprotons from extragalactic sources [14,20]. In some scenarios, the last two models can provide a p=p ratio increase up to the 10% level in the energy range under investigation.…”

Section: Cosmic-ray Antiprotonsmentioning

confidence: 99%

Measurement of the shadowing of high-energy cosmic rays by the Moon: A search for TeV-energy antiprotons

Achard

Адриани

Akker

et al. 2005

Astroparticle Physics

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The shadowing of high-energy cosmic rays by the Moon has been observed with a significance of 9.4 standard deviations with the L3 + C muon spectrometer at CERN. A significant effect of the Earth magnetic field is observed. Since 6 Supported by the German Bundesministerium fü r Bildung, Wissenschaft, Forschung und Technologie. 7 Supported by the Hungarian OTKA fund under contract numbers T019181, F023259 and T037350. 8 Supported by the National Natural Science Foundation of China. 9 Also supported by the Hungarian OTKA fund under contract number T026178. no event deficit on the east side of the Moon has been observed, an upper limit at 90% confidence level on the antiproton to proton ratio of 0.11 is obtained for primary energies around 1 TeV.

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“…10 −8 (Carr & McGibbon 1998) and 3 × 10 −9 , and from the number of antiprotons, 3 to 4 × 10 −9 (Maurin et al 2001;Barrau et al 2002). It is worth noting that our method is independent of the poorly known initial mass function of PBHs.…”

Section: Resultsmentioning

confidence: 99%

New constraints on the primordial black hole number density from Galactic γ-ray astronomy

Lehoucq¹,

Cassé

Casandjian³

et al. 2009

A&A

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Context. Primordial black holes are unique probes of cosmology, general relativity, quantum gravity and non standard particle physics. They open a new window on the very small scales in the early Universe and also can be considered as the ultimate particle accelerator in their last (explosive) moments since they are supposed to reach, very briefly, the Planck temperature. Aims. Upper limits on the primordial black hole number density of mass M = 5 × 10 14 g, the Hawking mass (born in the big-bang terminating their life presently), is determined comparing their predicted cumulative γ-ray emission, galaxy-wise, to the one observed by the EGRET satellite, once corrected for non thermal γ-ray background emission induced by cosmic ray protons and electrons interacting with light and matter in the Milky Way. Methods. A model with free gas emissivities is used to map the Galaxy in the 100 MeV photon range, where the peak of the primordial black hole emission is expected. The best gas emissivities and additional model parameters are obtained by fitting the EGRET data and are used to derive the maximum emission of the primordial black hole of the Hawking mass, assuming that they are distributed like the dark matter in the Galactic halo.Results. The bounds we obtain, depending on the dark matter distribution, extrapolated to the whole Universe (Ω PBH (M ) = 2.4×10 −10 to 2.6 × 10 −9 ) are more stringent than the previous ones derived from extragalactic γ-ray background and antiprotons fluxes, though less model dependent and based on more robust data. Conclusions. These new limits have interesting consequences on the theory of the formation of small structures in the Universe, since they are the only constraint on very small scale density fluctuations left by inflation. Significant improvements by data gathered by the FERMI γ-ray satellite are expected in the near future. The interest of a generalisation of this work beyond the standard particle model and in extradimensions is briefly alluded.

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Antiprotons from primordial black holes

Cited by 85 publications

References 53 publications

Cosmic positron signature from dark matter in the littlest Higgs model withTparity

Cosmic positron signature from dark matter in the littlest Higgs model withTparity

Measurement of the shadowing of high-energy cosmic rays by the Moon: A search for TeV-energy antiprotons

New constraints on the primordial black hole number density from Galactic γ-ray astronomy

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