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From Subatomic to Cosmic Scales: Simulating, Modelling, Analysing Binary Neutron...

From Subatomic to Cosmic Scales: Simulating, Modelling, Analysing Binary Neutron Star Mergers What is the nature of matter at supranuclear densities? What is the expansion rate of our Universe? These open questions of nuclear physics and cosmology can be answered with multi-messenger observation of merging binary neutron s... ver más

31/08/2028

1M€

Presupuesto del proyecto: 1M€

Líder del proyecto

UNIVERSITAET POTSDAM No se ha especificado una descripción o un objeto social para esta compañía.

TRL 4-5

Fecha límite participación Sin fecha límite de participación.

Financiación concedida El organismo HORIZON EUROPE notifico la concesión del proyecto el día 2022-12-15

ERC-2022-STG: ERC STARTING GRANTS Scope:Objectives

I+D

Cerrada hace 3 años

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No hay información privada compartida para este proyecto. Habla con el coordinador.

1 Participantes

1.50M€ | Lider

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Duración del proyecto: 68 meses Fecha Inicio: 2022-12-15
Fecha Fin: 2028-08-31

Líder del proyecto

UNIVERSITAET POTSDAM No se ha especificado una descripción o un objeto social para esta compañía.

TRL 4-5

Presupuesto del proyecto 1M€

Fecha límite de participación Sin fecha límite de participación.

Descripción del proyecto What is the nature of matter at supranuclear densities? What is the expansion rate of our Universe? These open questions of nuclear physics and cosmology can be answered with multi-messenger observation of merging binary neutron stars. The window to study these fascinating events has only recently been opened with the upgrades of gravitational-wave observatories and by combining gravitational-wave information with that of powerful telescopes in the electromagnetic spectrum - from infrared, to optical, to gamma-rays. In the near future, we expect numerous multi-messenger observations of compact binary systems. We are currently at a crossroads in which the development of accurate and robust theoretical models is crucial to keeping up with the development of experimental instrumentation. Without noticeable upgrades of our models, future analyses will be biased through modelling uncertainties. The proposed research project will focus on the development of theoretical models to interpret the binary neutron star coalescence and will pave the way for a thorough understanding of the merger process. Novel methods and algorithms that we will implement in our numerical-relativity code will allow us to study previously inaccessible regions of the binary neutron star parameter space with unprecedented accuracy. This accuracy in the determination of the gravitational-wave and electromagnetic emission from binary neutron star mergers is essential for connecting our theoretical computations with observational data. We will push for a publicly available framework for the simultaneous analysis of gravitational-wave and electromagnetic signals from binary neutron star mergers incorporating also nuclear-physics calculations, nuclear-physics experiments, and other astrophysical observations of isolated neutron stars. This framework will enable us to use upcoming detections to determine the neutron star radius and the Hubble constant.

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