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KILONOVA

Financiado

Probing r process nucleosynthesis through its electromagnetic signatures

The lightest chemical elements –Hydrogen and Helium– were created about a minute after the Big Bang. Elements up to Iron are forged by fusion reactions in stars. Heavy elements between Iron and Uranium are produced by a sequence o... ver más

31/12/2025

GSI

3M€

Presupuesto del proyecto: 3M€

Líder del proyecto

GSI HELMHOLTZZENTRUM FUR SCHWERIONENFORSCHUNG... No se ha especificado una descripción o un objeto social para esta compañía.

TRL 4-5

Ver 2 Participantes

Financiación concedida El organismo H2020 notifico la concesión del proyecto el día 2020-04-14

ERC-2019-ADG: ERC Advanced Grant

I+D

Cerrada hace 5 años

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2 Participantes

GSI

2.50M€ | Lider

SENSEI TECNOLOGIAS DE LA INF...

172.15K€ | Participante

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Duración del proyecto: 68 meses Fecha Inicio: 2020-04-14
Fecha Fin: 2025-12-31

Líder del proyecto

GSI HELMHOLTZZENTRUM FUR SCHWERIONENFORSCHUNG... No se ha especificado una descripción o un objeto social para esta compañía.

TRL 4-5

Presupuesto del proyecto 3M€

Descripción del proyecto The lightest chemical elements –Hydrogen and Helium– were created about a minute after the Big Bang. Elements up to Iron are forged by fusion reactions in stars. Heavy elements between Iron and Uranium are produced by a sequence of neutron captures and beta-decays known as rapid neutron capture or r process. The freshly synthesized r-process elements undergo radioactive decay through various channels depositing energy in the ejecta that powers an optical/infrared transient called kilonova whose basic properties like luminosity and its dependence on ejecta mass, velocity, radioactive energy input, and atomic opacities I contributed to determine for the first time. Our predictions have been dramatically confirmed by the observation of a kilonova electromagnetic transient associated with the gravitational wave signal GW170817 providing the first direct indication that r-process elements are produced in neutron-star mergers. Additional events are expected to be detected in the following years, representing a complete change of paradigm in r-process research as for the first time we will be confronted with direct observational data. To fully exploit such opportunity it is fundamental to combine an improved description of exotic neutron-rich nuclei involved in the r-process with sophisticated astrophysical simulations to provide accurate prediction of r-process nucleosynthesis yields and their electromagnetic signals to be confronted with observational data. Based on my broad knowledge and expertise in all the relevant areas, and the unique experimental capabilities of the GSI/FAIR facility, I am in prime position to advance our understanding of r-process nucleosynthesis and determine the contribution of mergers to the chemical enrichment of the galaxy in heavy elements.

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