Difference: FJPPLHighEnergyPhysics (9 vs. 10)
Revision 102017-06-30 - Main.GenevieveGilbert
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| < < | Several astrophysical or cosmological observations (evidences for dark matter, baryon asymmetry, inflation...) require an extension of the Standard Model of particle physics (so-called “beyond the standard model” (BSM) physics). Our project aims at investigating some theoretical ideas advanced to tackle several of the above-mentioned problems and their related phenomenological tests. In particular, we give high importance to the possibility to achieve the solution to several of these puzzles within the same (relatively simple) framework, as well as to the opportunity to establish links with the latest discoveries in the field of particle physics, notably Higgs and neutrino oscillations. For instance, the inflaton field may be related to the mass generation mechanism of right handed neutrinos, needed for neutrino oscillations, providing at the same time a dark matter candidate. We focus in particular on scenarios where the inflation and/or the additional degrees of freedom needed in a UV completion of the model are at or below the TeV scale, with obvious interesting implication for collider searches, at the energy frontier and/or at the intensity one. One such simple and attractive model is for instance the SM extension via a gauged U_{B-L}(1) symmetry, where the electroweak symmetry is radiatively broken by the Coleman-Weinberg mechanism. Some implications for small-field inflation inspired by this model have been already been analyzed in Ref. [1]. Others, notably for the reheating (at low temperatures), dark matter production, and possibly the associated Z’ phenomenology, are currently under scrutiny | |||||||
| > > | Several astrophysical or cosmological observations (evidences for dark matter, baryon asymmetry, inflation...) require an extension of the Standard Model of particle physics (so-called “beyond the standard model” (BSM) physics). The links between cosmology and particle physics heavily rely on the understanding on the history of the universe, which is often based on standard assumptions. For instance: an inflationary epoch produces a quasi-power law spectrum of perturbations (seeds of current structures) and ends in a radiation dominated period, during which conventional electroweak symmetry and QCD breaking happen as crossovers, according to the SM. Dark Matter is usually considered to be a particle relic, once in thermal contact with other SM species, etc. We are exploring possible departures from this simple picture. In the classically conformal extension of the SM, S. Iso, P. Serpico, and K. Shimada found that the chiral condensation in QCD can play an important role in the dynamics of the electroweak symmetry breaking. The phase transition becomes of the first order type and accordingly generates large gravitational waves that can be detected by future gravitational wave detectors [2]. Always related to gravitational waves, it is well known that the LIGO interferometers have detected their first sources of gravitational waves, from coalescences of binary black holes (BHs). While such binaries have long been considered an attractive candidate, the mechanism to produce them is not established, yet, in particular for such high masses (about 30 times the mass of the sun). It has also been conjectured that such BH may be of primordial origin. Their formation requires a significant departure from the simplest inflationary models, and at the same time it would lead to non-standard cosmological signatures, which can be searched for. This is another sector we are working on (notably k. Kohri with P. Serpico and V. Poulin) and some results are expected in the current year | |||||||
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French members : P. Serpico, | ||||||||
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| [1] S. Iso, K. Kohri and K. Shimada, "Dynamical fine-tuning of initial conditions for small field inflation," Phys. Rev. D 93, 084009 (2016) | ||||||||
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| < < | [arXiv:1511.05923] | |||||||
| > > | [arXiv:1511.05923] [2] S. Iso, P. D. Serpico and K. Shimada, "QCD-Electroweak first order phase transition in supercooled universe,'' arXiv:1704.04955 | |||||||
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