Resonant annihilation of long-lived massive colored particles through hadronic collisions

Kusakabe, Motohiko; Takesako, Tomohiro

doi:10.1103/physrevd.85.015005

Cited by 11 publications

(17 citation statements)

References 46 publications

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“…In this analysis, we adopt the estimation based on Refs. [34] and [36], which indicates O(10 −2 ) suppression, compared to the estimation by the naive dimensional analysis. If there is no such suppression, the DM abundance can be further reduced.…”

Section: Relic Abundancementioning

confidence: 99%

“…Finally, we briefly comment on the squark-squark bound state,qqq, for example. Roughly speaking, the formation cross section should be geometrical, but the Q-value is different from theq * q bound state formation process, and thus whether they are formed or not is not obvious [36]. However, once they are formed, the de-excitation and destruction processes will be similar to theq * q state case.…”

Section: Perturbative Annihilationmentioning

confidence: 99%

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How heavy can neutralino dark matter be?

Fukuda

Luo

Shirai

2019

J. High Energ. Phys.

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What is the upper limit of the mass of the neutralino dark matter whose thermal relic is consistent with the observation? If the neutralino dark matter and colored sparticles are extremely degenerated in mass, with a mass difference less than the QCD scale, the dark matter annihilation is significantly increased and enjoys the "second freeze-out" after the QCD phase transition. In this case, the neutralino dark matter with a mass much greater than 100 TeV can realize the correct dark matter abundance. We study the dark matter abundance and its detection in the case of such highly degenerated mass spectrum of the neutralino dark matter and colored supersymmetric particles.

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Section: Relic Abundancementioning

confidence: 99%

Section: Perturbative Annihilationmentioning

confidence: 99%

How heavy can neutralino dark matter be?

Fukuda

Luo

Shirai

2019

J. High Energ. Phys.

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“…The complication arises from interactions of colored NLSPs below the confinement temperature, which are described by poorly-understood non-perturbative strong dynamics [31,32]. Broadly speaking, colored NLSPs hadronize with quarks and gluons, forming heavy hadrons which then combine to form bound states containing multiple NLSPs.…”

Section: Relic Density Of Gravitinosmentioning

confidence: 99%

“…Alternatively, the NLSPs within a bound state may be unable to co-annihilate and then interact weakly with other bound states, maintaining a density similar to the perturbatively-calculated value. Estimates [32] of the relic density of a stable colored particle span a wide range of values, 4×10 −7 < Ωh 2 < 6×10 −3 for particle masses between 500 GeV and 3 TeV, depending on the species formed by hadronization. Although the effects of hadronization on the relic density of colored NLSPs are only understood qualitatively and may be strongly model-dependent, our model set is nearly unaffected by this uncertainty.…”

Section: Relic Density Of Gravitinosmentioning

confidence: 99%

The new look pMSSM with neutralino and gravitino LSPs

et al. 2012

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The pMSSM provides a broad perspective on SUSY phenomenology. In this paper we generate two new, very large, sets of pMSSM models with sparticle masses extending up to 4 TeV, where the lightest supersymmetric particle (LSP) is either a neutralino or gravitino. The existence of a gravitino LSP necessitates a detailed study of its cosmological effects and we find that Big Bang Nucleosynthesis places strong constraints on this scenario. Both sets are subjected to a global set of theoretical, observational and experimental constraints resulting in a sample of ∼ 225k viable models for each LSP type. The characteristics of these two model sets are briefly compared. We confront the neutralino LSP model set with searches for SUSY at the 7 TeV LHC using both the missing (MET) and non-missing E T ATLAS analyses. In the MET case, we employ Monte Carlo estimates of the ratios of the SM backgrounds at 7 and 8 TeV to rescale the 7 TeV data-driven ATLAS backgrounds to 8 TeV. This allows us to determine the pMSSM parameter space coverage for this collision energy. We find that an integrated luminosity of ∼ 5 − 20 fb −1 at 8 TeV would yield a substantial increase in this coverage compared to that at 7 TeV and can probe roughly half of the model set. If the pMSSM is not discovered during the 8 TeV run, then our model set will be essentially void of gluinos and lightest first and second generation squarks that are < ∼ 700 − 800 GeV, which is much less than the analogous mSUGRA bound. Finally, we demonstrate that non-MET SUSY searches continue to play an important role in exploring the pMSSM parameter space. These two pMSSM model sets can be used as the basis for investigations for years to come.

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“…We can regard excited states of 7 Be * X as effective paths to the GS if the transition rates are larger than their destruction rates. This treatment was utilized in an estimation of relic abundances of strongly interacting massive particles (SIMPs) after the cosmological color confinement by calculations for the annihilation of massive colored particles (Y 's) through a formation of resonant or bound states of (YȲ ) * [71]. From a comparison of rates for the 7 Be * X destruction [Eq.…”

Section: Transitions To the Gs 7 Bexmentioning

confidence: 99%

Be7charge exchange betweenBe3+7ion and an exotic long-lived negati

et al. 2013

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The existence of an exotic long-lived negatively charged massive particle, i.e., X − , during big bang nucleosynthesis can affect primordial light element abundances. Especially, the final abundance of 7 Li, mainly originating from the electron capture of 7 Be, has been suggested to reduce by the 7 Be destruction via the radiative X − capture of 7 Be followed by the radiative proton capture of the bound state of 7 Be and X − ( 7 BeX ). We suggest a new route of 7 BeX formation, that is the 7 Be charge exchange at the reaction of 7 Be 3+ ion and X − . The formation rate depends on the number fraction of 7 Be 3+ ion, the charge exchange cross section of 7 Be 3+ and the probability that produced excited states 7 Be * X are converted to the ground state. We estimate respective quantities affecting the 7 BeX formation rate, and find that this reaction pathway can be more important than ordinary radiative recombination of 7 Be and X − . The effect of the charge exchange reaction is then shown in a latest nuclear reaction network calculation. Quantum physical model calculations for related reactions are needed to precisely estimate the efficiency of this pathway in future.PACS numbers: 26.35.+c, 95.35.+d, 98.80.Cq, 98.80.Es I. INTRODUCTIONNew physics operating during the big bang nucleosynthesis (BBN) can be probed by observed light element abundances. Possible indications of new physics come from discrepancies between primordial abundances of 6 Li and 7 Li predicted in standard BBN (SBBN) model and those inferred from observations of metal-poor stars (MPSs). These MPSs exhibit a plateau-like abundance ratio, 7 Li/H = (1 − 2) × 10 −10 at low metallicities of [Fe/H]> −3 [1][2][3][4][5][6][7][8][9][10][11][12][13][14], and much lower at extremely low metallicities of [Fe/H]< −3 [15,16] [79]. The plateau abundance is a factor of 2-4 lower than the SBBN prediction for the baryon-to-photon ratio determined from the observation of the cosmic microwave background radiation with Wilkinson Microwave Anisotropy Probe (WMAP) (e.g., 7 Li/H=(5.24 +0.71−0.67 ) × 10 −10 [17]). This discrepancy indicates a need of some mechanism to decrease the 7 Li abundance. Although astrophysical processes such as the combination of atomic and turbulent diffusion in stellar atmospheres [18,19] may be a cause of the observed abundances, this is not yet established [20].In recent spectroscopic observations of MPSs, the lithium isotopic ratio of 6 Li/ 7 Li is also measured. A possible plateau abundance of 6 Li/H∼ 6 × 10 −12 has * Electronic address: motohiko@kau.ac.kr † Electronic address: kyungsik@kau.ac.kr ‡ Electronic address: cheoun@ssu.ac.kr § Electronic address: kajino@nao.ac.jp ¶ Electronic address: y.k@m.tohoku.ac.jp been suggested [4], which is about 1000 times higher than the SBBN prediction. Since an effect of convective motions in stellar atmospheres could cause asymmetries in atomic line profiles and consequently leads to an erroneous estimation of 6 Li abundance [21], the effect should be estimated. Even including this effect, high 6 Li ...

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Resonant annihilation of long-lived massive colored particles through hadronic collisions

Cited by 11 publications

References 46 publications

How heavy can neutralino dark matter be?

How heavy can neutralino dark matter be?

The new look pMSSM with neutralino and gravitino LSPs

Be7charge exchange betweenBe3+7ion and an exotic long-lived negati

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