ChemInform Abstract: THE TEMPERATURE DEPENDENCE OF THE RATIO K(D)/K(C) FOR ETHYL RADICALS

Hooper, David G.; Simon, M.; Back, M. H.

doi:10.1002/chin.197529135

Cited by 7 publications

(11 citation statements)

References 1 publication

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“…7. First, the dark sector may couple to the visible sector, communicating the visible sector supersymmetry breaking to the dark sector [129][130][131][132][133], as shown in the left panel of Fig. 7.…”

Section: A Hidden Sector Modelsmentioning

confidence: 99%

“…where F and M are the SUSY-breaking F -term and vev of the messenger field, respectively (see [135] for a review), α i ≡ g 2 i /(4π) are the SM gauge couplings, and C i are the quadratic Casimir invariants. If the messengers are likewise charged under a dark gauge group, U (1) X , supersymmetry breaking is communicated to the DM sector with strength [129,136]…”

mentioning

confidence: 99%

“…We now discuss a concrete model in the context of ADM, using the tools we just discussed [129,[131][132][133]. See [123] for more details of this model, though we outline the general In the left figure, SUSY breaking is communicated to the visible (SM) sector, which is then weakly communicated to the hidden sector via matter or gauge interactions, as in [129]. In the right figure [136] SUSY breaking is directly communicated to both hidden and visible sectors via gauge interactions, but the hidden sector is lighter because SUSY breaking is communicated more weakly to the DM than the baryons.…”

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confidence: 99%

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Asymmetric Dark Matter: Theories, signatures, and constraints

2014

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We review theories of Asymmetric Dark Matter (ADM), their cosmological implications and detection. While there are many models of ADM in the literature, our review of existing models will center on highlighting the few common features and important mechanisms for generation and transfer of the matter-anti-matter asymmetry between dark and visible sectors. We also survey ADM hidden sectors, the calculation of the relic abundance for ADM, and how the DM asymmetry may be erased at late times through oscillations. We consider cosmological constraints on ADM from the cosmic microwave background, neutron stars, the Sun, and brown and white dwarves. Lastly, we review indirect and direct detection methods for ADM, collider signatures, and constraints.

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Section: A Hidden Sector Modelsmentioning

confidence: 99%

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confidence: 99%

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confidence: 99%

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Asymmetric Dark Matter: Theories, signatures, and constraints

2014

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“…This is not surprising, as at energies above ∼100 GeV energy losses limit the number of sources that contribute to the electron cosmic ray spectrum; the cosmic ray electron spectrum at energies above a few hundred GeV is, therefore, likely to be dominated by only a small number of nearby sources. As a result, stochas-tic variations in the distribution of supernova remnants are expected to lead to local departures from the average cosmic ray spectrum found throughout the Milky Way (which may very well be a simple power-law) [26,69]. When the Fermi electron+positron spectrum is taken in combination with the positron fraction as measured by AMS, it is clear that more very high energy cosmic ray electrons are required than would be predicted using a simple power-law extrapolated from the low-energy spectrum.…”

Section: Annihilating Dark Mattermentioning

confidence: 99%

Dark matter and pulsar origins of the rising cosmic ray positron fraction in light of new data from the AMS

2013

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The rise of the cosmic ray positron fraction with energy, as first observed with high confidence by PAMELA, implies that a large flux of high energy positrons has been recently (or is being currently) injected into the local volume of the Milky Way. With the new and much more precise measurement of the positron fraction recently provided by AMS, we revisit the question of the origin of these high energy positrons. We find that while some dark matter models (annihilating directly to electrons or muons) no longer appear to be capable of accommodating these data, other models in which ∼1-3 TeV dark matter particles annihilate to unstable intermediate states could still be responsible for the observed signal. Nearby pulsars also remain capable of explaining the observed positron fraction. Future measurements of the positron fraction by AMS (using a larger data set), combined with their anticipated measurements of various cosmic ray secondary-to-primary ratios, may enable us to further discriminate between these remaining scenarios.PACS numbers: 95.85.Ry, 95.35.+d, 97.60.Gb; FERMILAB-PUB-13-090-A

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“…Much beneath an MeV, astrophysical and cosmological constraints allow only dark matter with ultra-weak couplings to quarks and leptons [38]. Between these boundaries (MeV − TeV), simple models of dark matter can account for its observed abundance through either thermal freeze-out or non-thermal mechanisms [39][40][41][42][43][44][45][46][47][48][49][50][51][52][53][54]. The conventional argument in favor of weak-scale ( 100 GeV) dark matter -that its annihilation through Standard Model (SM) forces alone suffices to explain the observed relic density -is dampened by strong experimental constraints on dark matter with significant couplings to the Z or Higgs bosons [12,55] and by the absence to date of evidence for new SM-charged matter at the LHC.…”

Section: Introductionmentioning

confidence: 99%

New electron beam-dump experiments to search for MeV to few-GeV dark matter

et al. 2013

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In a broad class of consistent models, MeV to few-GeV dark matter interacts with ordinary matter through weakly coupled GeV-scale mediators. We show that a suitable meter-scale (or smaller) detector situated downstream of an electron beam-dump can sensitively probe dark matter interacting via sub-GeV mediators, while B-factory searches cover the 1-5 GeV range. Combined, such experiments explore a well-motivated and otherwise inaccessible region of dark matter parameter space with sensitivity several orders of magnitude beyond existing direct detection constraints. These experiments would also probe invisibly decaying new gauge bosons ("dark photons") down to kinetic mixing of ∼ 10 −4 , including the range of parameters relevant for explaining the (g − 2)µ discrepancy. Sensitivity to other long-lived dark sector states and to new milli-charge particles would also be improved. arXiv:1307.6554v2 [hep-ph]

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ChemInform Abstract: THE TEMPERATURE DEPENDENCE OF THE RATIO K(D)/K(C) FOR ETHYL RADICALS

Cited by 7 publications

References 1 publication

Asymmetric Dark Matter: Theories, signatures, and constraints

Asymmetric Dark Matter: Theories, signatures, and constraints

Dark matter and pulsar origins of the rising cosmic ray positron fraction in light of new data from the AMS

New electron beam-dump experiments to search for MeV to few-GeV dark matter

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