COCO2CASA

Modeling Stellar Collapse and Explosion: Evolving Progenitor Stars to Supernova Remnants

Coordinatore	MAX PLANCK GESELLSCHAFT ZUR FOERDERUNG DER WISSENSCHAFTEN E.V.    more Spiacenti, non ci sono informazioni su questo coordinatore. Contattare Fabio per maggiori infomrazioni, grazie.
Nazionalità Coordinatore	Germany [DE]
Totale costo	2˙898˙600 €
EC contributo	2˙898˙600 €
Programma	FP7-IDEAS-ERC Specific programme: "Ideas" implementing the Seventh Framework Programme of the European Community for research, technological development and demonstration activities (2007 to 2013)
Code Call	ERC-2013-ADG
Funding Scheme	ERC-AG
Anno di inizio	2014
Periodo (anno-mese-giorno)	2014-02-01   -   2019-01-31

 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: Dr. Nome: Hans-Thomas Cognome: Janka Email: send email Telefono: +49 89 30000 2228 Fax: +49 89 30000 2235	DE (MUENCHEN)	hostInstitution	2˙898˙600.00
2	MAX PLANCK GESELLSCHAFT ZUR FOERDERUNG DER WISSENSCHAFTEN E.V.  Organization address address: Hofgartenstrasse 8 city: MUENCHEN postcode: 80539 contact info Titolo: Mr. Nome: Bernhard Cognome: Scheiner Email: send email Telefono: +49 89 300003303 Fax: +49 89 300003243	DE (MUENCHEN)	hostInstitution	2˙898˙600.00

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 Obiettivo del progetto (Objective)

'This project intends to make groundbreaking progress towards the solution of one of the most pestering and long-standing riddles of stellar astrophysics, namely the question how massive stars explode as supernovae (SNe). State-of-the-art simulations in two dimensions (2D) now yield neutrino-powered (through underenergetic) explosions for a growing variety of progenitors and thus support the delayed neutrino-heating mechanism. However, sophisticated, fully self-consistent, 3D simulations are still lacking, the spherical symmetry of the progenitor star models is becoming a serious handicap, and better exploitation of observational constraints of the SN mechanism is urgently needed. For these reasons we plan a novel, comprehensive modeling approach, in which 3D hydrodynamics including all relevant microphysics will not only be employed for the launch phase of the SN blast wave by neutrino-energy deposition. Different from previous initiatives, 3D hydrodynamics will also be applied to the final stages of convective shell burning in the progenitor core before collapse in order to derive --for the first time-- self-consistent, multidimensional progenitor data for adopting them as initial conditions in the SN modeling. Moreover, the 3D explosion simulations will be continued consistently through the long-time evolution of the SN outburst into the gaseous remnant phase. This challenging approach promises fundamentally new insights into the processes that trigger and shape SN explosions and will revise our understanding of how SNe depend on the properties of their progenitor stars. Moreover, heading for a direct comparison of the derived theoretical models with nearby young SN remnants like Crab, Cassiopeia A, and SN 1987A, whose 3D morphology and composition are currently unfolded in stunning detail by multiwavelength observations, the project will lay the foundations of a powerful, innovative, and so far not exploited way of probing the physics deep inside the SN core.'