Antinucleons from decaying gravitinos in supersymmetric cosmology

Halm, I.

doi:10.1016/0370-2693(87)91638-8

Cited by 5 publications

(4 citation statements)

References 29 publications

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“…However, such a large gravitino mass cannot be accomodated in (minimal) supergravity models without destabilizing the hierarchy. Other constraints on the gravitino abundance follow from examination of the effects of the annihilation of antiprotons produced in the decay chain 3 2 → gg, g → q q γ (Khlopov and , Ellis et al 1985b, Halm 1987, Dominguez-Tenreiro 1987) but these are not as restrictive as those given above. The effects of the decay 3 2 → ν ν have been studied…”

Section: The Gravitino Problem Baryogenesis and Inflationmentioning

confidence: 99%

“…When the x particle decays into energetic quarks or gluons, these fragment into hadronic showers which interact with the ambient nucleons thus changing their relative abundances. (The alteration of elemental abundances by direct annihilation with antinucleons has also been considered (e.g Khlopov and Linde 1984, Ellis et al 1985b, Halm 1987, Dominguez-Tenreiro 1987; however Dimopoulos et al (1988) have shown that the effect of the hadronic showers is far more important.) If such hadronic decays occur during nucleosyntheis, the neutron-to-proton ratio is increased resulting in the production of more D and 4 He (Reno and Seckel 1988).…”

Section: 'Invisible' Decaysmentioning

confidence: 99%

“…Other constraints on the gravitino abundance follow from examination of the effects of the annihilation of antiprotons produced in the decay chain 3/2 →gg,g → qqγ (Khlopov and Linde 1984, Ellis et al 1985b, Halm 1987, Dominguez-Tenreiro 1987) but these are not as restrictive as those given above. The effects of the decay 3/2 → νν have been studied by de Laix and Scherrer (1993).…”

Section: The Gravitino Problem Baryogenesis and Inflationmentioning

confidence: 99%

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Big bang nucleosynthesis and physics beyond the standard model

1996

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Abstract. The Hubble expansion of galaxies, the 2.73 K blackbody radiation background and the cosmic abundances of the light elements argue for a hot, dense origin of the universe -the standard Big Bang cosmology -and enable its evolution to be traced back fairly reliably to the nucleosynthesis era when the temperature was of O(1) MeV corresponding to an expansion age of O(1) sec. All particles, known and hypothetical, would have been created at higher temperatures in the early universe and analyses of their possible effects on the abundances of the synthesized elements enable many interesting constraints to be obtained on particle properties. These arguments have usefully complemented laboratory experiments in guiding attempts to extend physics beyond the Standard SU (3) c ⊗SU (2) L ⊗U (1) Y Model, incorporating ideas such as supersymmetry, compositeness and unification. We first present a pedagogical account of relativistic cosmology and primordial nucleosynthesis, discussing both theoretical and observational aspects, and then proceed to examine such constraints in detail, in particular those pertaining to new massless particles and massive unstable particles. Finally, in a section aimed at particle physicists, we illustrate applications of such constraints to models of new physics.

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Section: The Gravitino Problem Baryogenesis and Inflationmentioning

confidence: 99%

Section: 'Invisible' Decaysmentioning

confidence: 99%

Section: The Gravitino Problem Baryogenesis and Inflationmentioning

confidence: 99%

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Big bang nucleosynthesis and physics beyond the standard model

1996

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“…Much of the early work on BBN with antimatter [1,[20][21][22] was either in the context of a baryon symmetric universe [20] or for a homogeneous injection of antimatter through some decay process [22].…”

Section: Bbn With Antimattermentioning

confidence: 99%

Antimatter regions in the early universe and big bang nucleosynthesis

Kurki-Suonio

Sihvola

2000

Phys. Rev. D

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We have studied big bang nucleosynthesis in the presence of regions of antimatter. Depending on the distance scale of the antimatter region, and thus the epoch of their annihilation, the amount of antimatter in the early universe is constrained by the observed abundances. Small regions, which annihilate after weak freezeout but before nucleosynthesis, lead to a reduction in the 4 He yield, because of neutron annihilation. Large regions, which annihilate after nucleosynthesis, lead to an increased 3 He yield. Deuterium production is also affected but not as much. The three most important production mechanisms of 3 He are 1) photodisintegration of 4 He by the annihilation radiation, 2)p 4 He annihilation, and 3)n 4 He annihilation by "secondary" antineutrons produced in 4 He annihilation. Althoughp 4 He annihilation produces more 3 He than the secondaryn 4 He annihilation, the products of the latter survive later annihilation much better, since they are distributed further away from the annihilation zone.PACS numbers: 26.35.+c, 98.80.Ft, 98.80.Cq, 25.43.+t HIP-2000-31/TH

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