EURO_GRANOT

Exploring Ultra-Relativistic Outflows

Coordinatore	THE UNIVERSITY OF HERTFORDSHIRE HIGHER EDUCATION CORPORATION    more  Organization address address: COLLEGE LANE city: HATFIELD postcode: AL10 9AB contact info Titolo: Prof. Nome: James Cognome: Hough Email: send email Telefono: -286163 Fax: -286177
Nazionalità Coordinatore	United Kingdom [UK]
Totale costo	100˙000 €
EC contributo	100˙000 €
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-2007-4-3-IRG
Funding Scheme	MC-IRG
Anno di inizio	2007
Periodo (anno-mese-giorno)	2007-09-01   -   2011-08-31

 Partecipanti

#	participant	country	role	EC contrib. [€]
1	THE UNIVERSITY OF HERTFORDSHIRE HIGHER EDUCATION CORPORATION  Organization address address: COLLEGE LANE city: HATFIELD postcode: AL10 9AB contact info Titolo: Prof. Nome: James Cognome: Hough Email: send email Telefono: -286163 Fax: -286177	UK (HATFIELD)	coordinator	0.00

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 Obiettivo del progetto (Objective)

'Relativistic outflows appear in a wide variety of astrophysical sources, from Galactic micro-quasars to cosmological gamma-ray bursts (GRBs) and active galactic nuclei (AGN). In most cases the relativistic outflow is thought to arise from accretion onto a black hole, while neutron-stars are also known to produce relativistic outflows (either in the form of a steady wind or an impulsive ejection of plasmoids). Such relativistic outflow sources are thought to accelerate the highest energy cosmic rays, and are expected to be important sources of high-energy neutrinos and gravitational waves for upcoming detectors. Furthermore, they can probe strong field gravity, large densities and magnetic fields, and may have a strong effect on their environment. Thus, a good understanding of their physics can have many important implications. I plan to study several different aspects of ultra-relativistic outflows, which may help shed light on their underlying physics: (i) the acceleration of an impulsive highly-magnetized relativistic outflow, its interaction with the external medium, as well as the energy dissipation and emission mechanism within the outflow. These have been investigated so far mainly in quasi-steady state long-lived sources, and the differences for impulsive short-lived outflows is of great importance, and particularly relevant for GRBs; (ii) time dependent opacity effects in impulsive relativistic sources – they lead to different observed properties compared to quasi-steady state sources, and probes the emission site and the Lorentz factor of the outflow, and thus its composition (which is very poorly constrained); this is relevant to the prompt gamma-ray emission in GRBs, as well as to flares in Blazars, micro-quasars and GRBs; (iii) The stability properties of relativistic shocks – these develop is relativistic outflow sources and may effect their observed properties, but have not been investigated in much detail so far, as their Newtonian counterparts.'