MOMENTUM

Angular momentum transfer in galaxy formation and evolution

Coordinatore	OBSERVATOIRE DE PARIS    more Spiacenti, non ci sono informazioni su questo coordinatore. Contattare Fabio per maggiori infomrazioni, grazie.
Nazionalità Coordinatore	France [FR]
Totale costo	2˙316˙000 €
EC contributo	2˙316˙000 €
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-2010-AdG_20100224
Funding Scheme	ERC-AG
Anno di inizio	2011
Periodo (anno-mese-giorno)	2011-01-01   -   2015-12-31

 Partecipanti

#	participant	country	role	EC contrib. [€]
1	OBSERVATOIRE DE PARIS  Organization address address: AVENUE DE L OBSERVATOIRE 61 city: PARIS postcode: 75014 contact info Titolo: Mr. Nome: Mathieu Cognome: Jacques Email: send email Telefono: +33 1 40512125 Fax: +33 1 40512207	FR (PARIS)	hostInstitution	2˙316˙000.00
2	OBSERVATOIRE DE PARIS  Organization address address: AVENUE DE L OBSERVATOIRE 61 city: PARIS postcode: 75014 contact info Titolo: Prof. Nome: Françoise Cognome: Combes Email: send email Telefono: +33 1 40512077 Fax: +33 1 40512002	FR (PARIS)	hostInstitution	2˙316˙000.00

Mappa

 Word cloud

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

 Obiettivo del progetto (Objective)

'The project is dedicated to follow angular momentum within structures over a wide range of scales, to trace galaxy formation and the history of mass assembly. Angular momentum is a key parameter to determine galaxy morphology and kinematics. After primordial spin-up by tidal torques, the subsequent evolution may help to understand galaxy formation, although numerical models fail to reproduce large disk galaxies today, by lack of angular momentum. The project will focus on three areas: -- (i) detailed angular momentum transfer due to non-axisymmetric features, such as bars and spirals, in early galaxies, submitted to internal dynamical processes, but also external matter accretion --- (ii) census of angular momentum exchanges during galaxy interactions, transformation from orbital to internal spin, and exchange between the various components, role of the environment on the density of angular momentum, through cosmic filaments, and formation of large-scale structures -- (iii) efficient fueling of super-massive black holes (SMBH) in the early universe, through angular momentum transfer, and study of complex feedback processes, in particular around bright cluster galaxies, at the centre of cooling flows. To address these three issues, we will carry on complementary simulations, with the best state-of-the art codes, tree-SPH, multi-phase including sticky particles, or Eulerian AMR code. The complex baryonic physics will be modelled, and comparisons made while varying methods and physical parameters. The highest resolution will be used to trace angular momentum transfer and resonances in idealised galaxies, but boundary conditions will be obtained from cosmological large-scale simulations. At every step, the simulations will be confronted to observations.'