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CRAGSMAN SIGNED

The Impact of Cosmic Rays on Galaxy and Cluster Formation

Total Cost €

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EC-Contrib. €

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Partnership

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 CRAGSMAN project word cloud

Explore the words cloud of the CRAGSMAN project. It provides you a very rough idea of what is the project "CRAGSMAN" about.

physics    star    cosmic    feedback    rays    cosmological    gas    ray    clusters    galaxies    hydrodynamic    galaxy    turbulence    simulations    magneto   

Project "CRAGSMAN" data sheet

The following table provides information about the project.

Coordinator
LEIBNIZ-INSTITUT FUR ASTROPHYSIK POTSDAM (AIP) 

Organization address
address: AN DER STERNWARTE 16
city: POTSDAM
postcode: 14482
website: www.aip.de

contact info
title: n.a.
name: n.a.
surname: n.a.
function: n.a.
email: n.a.
telephone: n.a.
fax: n.a.

 Coordinator Country Germany [DE]
 Total cost 2˙000˙000 €
 EC max contribution 2˙000˙000 € (100%)
 Programme 1. H2020-EU.1.1. (EXCELLENT SCIENCE - European Research Council (ERC))
 Code Call ERC-2014-CoG
 Funding Scheme /ERC-COG
 Starting year 2016
 Duration (year-month-day) from 2016-04-01   to  2021-03-31

 Partnership

Take a look of project's partnership.

# participants  country  role  EC contrib. [€] 
1    LEIBNIZ-INSTITUT FUR ASTROPHYSIK POTSDAM (AIP) DE (POTSDAM) coordinator 1˙783˙464.00
2    HITS GGMBH DE (HEIDELBERG) participant 216˙535.00

Mappa

 Project objective

'Understanding the physics of galaxy formation is arguably among the greatest problems in modern astrophysics. Recent cosmological simulations have demonstrated that 'feedback' by star formation, supernovae and active galactic nuclei appears to be critical in obtaining realistic disk galaxies, to slow down star formation to the small observed rates, to move gas and metals out of galaxies into the intergalactic medium, and to balance radiative cooling of the low-entropy gas at the centers of galaxy clusters. This progress still has the caveat that 'feedback' was modeled empirically and involved tuning to observed global relations, substantially weakening the predictive power of hydrodynamic simulations. More problematic, these simulations neglected cosmic rays and magnetic fields, which provide a comparable pressure support in comparison to turbulence in our Galaxy, and are known to couple dynamically and thermally to the gas. Building on our previous successes in investigating these high-energy processes, we propose a comprehensive research program for studying the impact of cosmic rays on the formation of galaxies and clusters. To this end, we will study cosmic-ray propagation in magneto-hydrodynamic turbulence and improve the modeling of the plasma physics. This will enable us to perform the first consistent magneto-hydrodynamical and cosmic-ray simulations in a cosmological framework, something that has just now become technically feasible. Through the use of an advanced numerical technique that employs a moving mesh for calculating hydrodynamics, we will achieve an unprecedented combination of accuracy, resolution and physical completeness. We complement our theoretical efforts with a focused observational program on the non-thermal emission of galaxies and clusters, taking advantage of new capabilities at radio to gamma-ray wavelengths and neutrinos. This promises important and potentially transformative changes of our understanding of galaxy formation.'

 Work performed, outcomes and results:  advancements report(s) 

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