Synthesis and Aromatic Nucleophilic N—N, N—S and N—O Exchange Reactions of N,N‐Dimethyl‐2‐trifluoroacetyl‐1‐naphthylamine.

Okada, Etsuji; Otsuki, Yoshihiro; Shinohara, Megumi; Médebielle, Maurice; Shimizu, Yuhei; Takeuchi, Hiroshi

doi:10.1002/chin.200318085

Cited by 7 publications

(11 citation statements)

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“…In figure 16 we show the scales probed for α = 1, v w = 1 and β/H * = 1.3 log[T * /M P for all three contributions. A phase transition with a peak frequency visible by LIGO/VIRGO can be motivated by vacuum stability [367], split supersymmetry [368], a Pati-Salam transition [369] or neutrino masses [370,371]. Lisa probes both the electroweak phase transition [232,284,341,[372][373][374][375][376][377][378][379][380][381][382][383][384][385][386][387][388], dark phase transitions [364,[389][390][391][392][393][394][395] other low scale symmetry breaking [396][397][398][399], multistep transitions [232] and multistep phase transitions [231,232] whereas pulsar timing arrays can probe supercooled electroweak phase transitions and the QCD phase transition [304,400,401].…”

Section: Turbulencementioning

confidence: 99%

Review of cosmic phase transitions: their significance and experimental signatures

Mazumdar

White²

2019

Rep. Prog. Phys.

206

195

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The study of cosmic phase transitions are of central interest in modern cosmology. In the standard model of cosmology the Universe begins in a very hot state, right after at the end of inflation via the process of reheating/preheating, and cools to its present temperature as the Universe expands. Both new and existing physics at any scale can be responsible for catalyzing either first, second or cross over phase transition, which could be either thermal or non-thermal with a potential observable imprints. Thus this field prompts a rich dialogue between gravity, particle physics and cosmology. It is all but certain that at least two cosmic phase transitions have occurred -the electroweak and the QCD phase transitions. The focus of this review will be primarily on phase transitions above such scales, We review different types of phase transitions that can appear in our cosmic history, and their applications and experimental signatures in particular in the context of exciting gravitational waves, which could be potentially be constrained by LIGO/VIRGO, Kagra, and eLISA.Let us briefly summarize the early Universe cosmology in chronological order. How the Universe began remains a profound question, for which we do not have direct experimental evidence yet. Nonetheless, we can speculate based on sound physical arguments and the observations confirmed by the detection of cosmic microwave background (CMB) radiation [46,47]. How did the Universe begin?Einstein's theory of gravity (GR) is extremely successful in the infrared (IR) matching of all possible observables [48], including the recent discovery of gravitational waves from mergers of two blackholes [49], and binary neutron star mergers [50]. However at short distances and small time scales, i.e. in the ultraviolet (UV), GR has pathologies, besides being a non-renormalizable theory, GR introduces cosmological and blackhole singularities, see [51], and in some cases naked singularities, see [52]. In GR, our Universe has a distinct starting point, a singular spacetime -as long as all the standard energy conditions are always satisfied, i.e. strong, weak, and null energy conditions, see [51]. It is possible to address the cosmological singularity problem without violating the matter energy conditions by weakening the gravitational interaction in the UV. This can happen in ghost free infinite derivative gravity inspired from string field theory [53,54]. There could be two consequences for such study; one could be a realization of a non-singular bounce [55,56], and the other scenario would be that Universe could be frozen in time in the UV, such that the Universe becomes conformal as t → 0 [57]. Bouncing cosmologies and cosmological density perturbations have been reviewed in this nice review [58,59]. There is a strong indication that this non-singular initial phase of the Universe has a key role to play towards understanding the subsequent phases of the Universe such as cosmic inflation, horizon, homogeneity and isotropy of the Universe , to create appropriate initial co...

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Section: Turbulencementioning

confidence: 99%

Review of cosmic phase transitions: their significance and experimental signatures

Mazumdar

White²

2019

Rep. Prog. Phys.

206

195

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“…A general requirement is that DM particles should couple with electrons (leptons) instead of quarks. A simple extension is to add a U(1) X symmetry to the standard model, and the DM annihilate into electrons (leptons) via the new gauge boson mediator, e.g., a Z ′ [95][96][97][98][99][100][101][102][103][121][122][123][124]. In the fermion DM case, the Dirac type is more natural as its cross section is s-wave dominant for the s-channel annihilation process χχ → Z ′ → ff .…”

Section: Discussion On the Tentative 14 Tev Structurementioning

confidence: 99%

Dark Matter Particle Explorer observations of high-energy cosmic ray electrons plus positrons and their physical implications

Yuan

Liu

2018

Sci. China Phys. Mech. Astron.

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The DArk Matter Particle Explorer (DAMPE) is a satellite-borne, high-energy particle and γ-ray detector, which is dedicated to indirectly detecting particle dark matter and studying high-energy astrophysics. The first results about precise measurement of the cosmic ray electron plus positron spectrum between 25 GeV and 4.6 TeV were published recently. The DAMPE spectrum reveals an interesting spectral softening arount 0.9 TeV and a tentative peak around 1.4 TeV. These results have inspired extensive discussion. The detector of DAMPE, the data analysis, and the first results are introduced. In particular, the physical interpretations of the DAMPE data are reviewed. PACS numbers: 95.35.+d,95.85.Ry,96.50.sb * yuanq@pmo.ac.cn 1 See also earlier hints from HEAT and AMS measurements [16,17].

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“…This new analyses also disfavour the possibility of the previous proposition of ∼ 10 GeV DM annihilating solely into ττ channels. ‡ There are several attempts (Logan 2011;Buckley et al 2011b;Zhu 2011;Marshall & Primulando 2011;Boucenna & Profumo 2011;Buckley et al 2011a;Hooper et al 2012;Buckley et al 2013;Anchordoqui & Vlcek 2013;Guo et al 2014;Yu 2014;Cahill-Rowley et al 2015;Borah & Dasgupta 2015;Banik & Majumdar 2014;Okada & Seto 2014a;Cheung et al 2014;Basak & Mondal 2014;Berlin et al 2014a;Ghosh et al 2015;Ko et al 2014;Balzs & Li 2014;Agrawal et al 2014b,c;Izaguirre et al 2014;Cerdeo et al 2014;Ipek et al 2014;Boehm et al 2014a;Wang & Han 2014;Fields et al 2014;Arina et al 2015;Huang et al 2014;Ko & Tang 2015;Agrawal et al 2014a;Okada & Seto 2014b;Boehm et al 2014b;Alves et al 2014;Berlin et al 2014b;Abdullah et al 2014;Martin et al 2014;Cline et al 2014;Detmold et al 2014;…”

Section: Introductionmentioning

confidence: 99%

CONFRONTING GALACTIC AND EXTRAGALACTIC γ -RAYS OBSERVED BY FERMI -LAT WITH ANNIHILATING DARK MATTER IN AN INERT HIGGS DOUBLET MODEL

Modak

Majumdar

2015

ApJS

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In this thorough study we focus on the indirect detection of Dark Matter (DM) through the confrontation of unexplained galactic and extragalactic γ-ray signatures for a low mass DM model. For this, we consider a simple Higgs-portal DM model, namely, the inert Higgs doublet model (IHDM) where the Standard Model is extended with an additional complex SU(2) L doublet scalar. The stability of the DM candidate in this model, i.e., the lightest neutral scalar component of the extra doublet, is ensured by imposing discrete Z 2 symmetry. The reduced-χ 2 analysis with the theoretical, experimental and observational constraints suggests the best-fit value of DM mass in this model to be ∼ 63.5 GeV. We analyse the anomalous GeV γ-ray excess from Galactic Centre in light of the best-fit IHDM parameters. We further check the consistency of the best-fit IHDM parameters with the Fermi-LAT obtained limits on photon flux for 18 Milky Way dwarf spheroidal satellite galaxies (dSphs) known to be mostly dominated by DM. Also since the γ-ray signal from DM annihilation is assumed to be embedded within the extragalactic γ-ray background (EGB), the theoretical calculations of photon flux for the best-fit parameter point in the IHDM framework are compared with the Fermi-LAT results for diffuse and isotropic EGB for different extragalactic and astrophysical background parametrisations. We show that the low mass DM in IHDM framework can satisfactorily confront all the observed continuum γ-ray fluxes originated from galactic as well as extragalactic sources. The extensive analysis performed in this work is valid for any Higgs-portal model with DM mass in the ballpark of that considered in this work. * kamakshya.modak@saha.ac.in † debasish.majumdar@saha.ac.in ‡ cosmic ray positron data also disfavour the possibility of DM annihilating into τ lepton pairs with the proposed mass of DM (∼ 10 GeV) and annihilation cross-section to accommodate GeV gamma-ray excess.

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Synthesis and Aromatic Nucleophilic N—N, N—S and N—O Exchange Reactions of N,N‐Dimethyl‐2‐trifluoroacetyl‐1‐naphthylamine.

Cited by 7 publications

References 1 publication

Review of cosmic phase transitions: their significance and experimental signatures

Review of cosmic phase transitions: their significance and experimental signatures

Dark Matter Particle Explorer observations of high-energy cosmic ray electrons plus positrons and their physical implications

CONFRONTING GALACTIC AND EXTRAGALACTIC γ -RAYS OBSERVED BY FERMI -LAT WITH ANNIHILATING DARK MATTER IN AN INERT HIGGS DOUBLET MODEL

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