DYNACOR

From the Sun to stars - Interplay between dynamo and corona

 Coordinatore MAX PLANCK GESELLSCHAFT ZUR FOERDERUNG DER WISSENSCHAFTEN E.V. 

 Organization address address: Hofgartenstrasse 8
city: MUENCHEN
postcode: 80539

contact info
Titolo: Mr.
Nome: Detlef
Cognome: Steinmann
Email: send email
Telefono: +49 551 384 979 285
Fax: +49 551 384 979 8285

 Nazionalità Coordinatore Germany [DE]
 Totale costo 161˙968 €
 EC contributo 161˙968 €
 Programma FP7-PEOPLE
Specific programme "People" implementing the Seventh Framework Programme of the European Community for research, technological development and demonstration activities (2007 to 2013)
 Code Call FP7-PEOPLE-2013-IEF
 Funding Scheme MC-IEF
 Anno di inizio 2015
 Periodo (anno-mese-giorno) 2015-01-01   -   2016-12-31

 Partecipanti

# participant  country  role  EC contrib. [€] 
1    MAX PLANCK GESELLSCHAFT ZUR FOERDERUNG DER WISSENSCHAFTEN E.V.

 Organization address address: Hofgartenstrasse 8
city: MUENCHEN
postcode: 80539

contact info
Titolo: Mr.
Nome: Detlef
Cognome: Steinmann
Email: send email
Telefono: +49 551 384 979 285
Fax: +49 551 384 979 8285

DE (MUENCHEN) coordinator 161˙968.80

Mappa


 Word cloud

Esplora la "nuvola delle parole (Word Cloud) per avere un'idea di massima del progetto.

coronal    numerical    solar    dynamo    stellar    dynamos    corona    models    magnetic    stars    simulations    relation    fundamental    events    interior    interpretation    first   

 Obiettivo del progetto (Objective)

'Most stars show strong magnetic fields on their surfaces and sustain a hot outer atmosphere, the corona. Two of the fundamental problems in stellar astrophysics are how the stars generate their magnetic field, and how they manage to heat the corona to temperatures of two million K, well in excess of the surface. I will address these problems by performing local and global numerical simulations. These include the stellar interior and an overlaying corona, which are evolved self-consistently by solving the magnetohydrodynamic equations using high performance computing. First results of such novel simulations show that the dynamo benefits substantially from the presence of a corona leading to a stronger amplification of the magnetic field inside the star and that the dynamo can drive dynamic events in the corona. For a more complete understanding of the coupled dynamo-corona system, further steps towards more realistic models have to be taken. The overall goal of the proposed project can be subdivided into three major parts: (1) understand fundamental properties of stellar dynamos using accurate mean-field models of the direct numerical simulations, (2) investigate the influence of the coronal envelope on stellar dynamos and stellar interiors, (3) determine the role of stellar dynamos for the formation and evolution of coronal structures. This study will have a major impact on the fundamental understanding of solar and stellar activity cycles, which is pivotal for interpretation of stellar observations. In particular this concerns the description of the solar and stellar dynamo processes, the formation of space-weather events and the coronal heating mechanisms. Modeling the exact relation between stellar parameters, dynamos in the interior and coronal properties will for the first time provide a clear interpretation of observable atmospheric quantities for a large range of stars, for example the relation of rotation rate and stellar X-ray luminosity.'

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