Wolfgang Pauli Institute (WPI) Vienna |
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| Oliver Hahn (Obs Nice) | Fri, 21. Feb 20, 11:15 | |
| Cosmological Structure Formation: Numerics and Theory, State of the Art and Open Problems | ||
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| Robin Kaiser (INLPH Nice) | Fri, 21. Feb 20, 11:45 | |
| Photon –Atom Interactions: from cold atoms to astrophysics | ||
Atomic physics experiments, based on hot vapors or laser-cooled atomic samples, may be useful to simulate some astrophysical problems, where radiation pressure, radiative transport or light amplification are involved. I will present some ongoing experimental efforts in Nice and discuss spontaneous self-organisation with light-induced long-range forces. | ||
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| Sebastian Erne (VCQ Wien) | Fri, 21. Feb 20, 14:30 | |
| Analog simulators for early universe cosmology: from false vacuum decay to reheating | ||
Designing effective field theories in a laboratory setup has gained increasing attention over the last years and lies at the heart of analog-gravity experiments. Probing the validity of these effective models constitutes an essential step towards (quantum) simulators of otherwise inaccessible systems. Focusing on its applications for early universe cosmological problems, I report on the opportunities, validation, and limitations of analog classical and quantum simulators for (Quantum) Field Theory in curved and time-dependent spacetimes, in particular to cosmic inflation. As specific examples, I will discuss applications of single and multi-component quantum fluids and classical two-fluid systems in strong gradient magnetic fields. | ||
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| Cornelius Rampf (Obs Nice) | Fri, 21. Feb 20, 15:00 | |
| Singularities in cosmological Vlasov-Poisson and quantum picture | ||
The evolution of cold dark matter (CDM) is governed by the cosmological Vlasov–Poisson equations. As it is well-known, the gravitational collapse of CDM leads to infinite-density caustics that seed the primordial dark-matter halos in the cosmic large-scale structure. Focusing on the one-dimensional case, I report a landscape of so far unknown singularities in the particle acceleration that emerge after the first crossing of particle trajectories. These singular features may be regulated by assuming a finite temperature for dark matter, which, to some extend, simplifies the numerical computation but complicates the theoretical modelling. Alternatively, singular features are naturally tamed in semiclassical, Schrödinger-like descriptions for the large-scale structure which I will discuss as well. | ||
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