We propose a new inflationary toy model that produces two episodes of phase transitions. With the first one, super-horizon-sized bubbles are nucleated, which are seen from inside as open universes, thereby reconciling inflation with the recent observations of a low Ω0. With the second transition, a distribution of sub-horizon voids, of sizes typically around 10–100 Mpc/h are generated inside the open universes. These primordial voids can be the seeds of the present large scale voids that are detected in redshift surveys, and provide a non-Gaussian signal on the microwave background. The model realizes this sequence along the same slow-rolling path, by modulating the energy difference between the vacuum states. In this model, that we call extended Bubbly CDM, openness and bubblyness, rather than flatness and homogeneity, are the main products of inflation.

Extended BCDM / Occhionero, F.; Baccigalupi, C.; Amendola, L.. - 476:1(1999), pp. 174-185. (Intervento presentato al convegno 3K cosmology tenutosi a Roma nel October 1998) [10.1063/1.59323].

Extended BCDM

Baccigalupi, C.;
1999-01-01

Abstract

We propose a new inflationary toy model that produces two episodes of phase transitions. With the first one, super-horizon-sized bubbles are nucleated, which are seen from inside as open universes, thereby reconciling inflation with the recent observations of a low Ω0. With the second transition, a distribution of sub-horizon voids, of sizes typically around 10–100 Mpc/h are generated inside the open universes. These primordial voids can be the seeds of the present large scale voids that are detected in redshift surveys, and provide a non-Gaussian signal on the microwave background. The model realizes this sequence along the same slow-rolling path, by modulating the energy difference between the vacuum states. In this model, that we call extended Bubbly CDM, openness and bubblyness, rather than flatness and homogeneity, are the main products of inflation.
1999
3K cosmology
476
1
174
185
1563968479
American Institute of Physics
Occhionero, F.; Baccigalupi, C.; Amendola, L.
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/20.500.11767/15299
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