SHALOM

Explosive phenomena in the Universe: Gamma-Ray Bursts and SuperNovaRemnants as high-energy particle acceleration sites

Coordinatore	THE HEBREW UNIVERSITY OF JERUSALEM.    more  Organization address address: GIVAT RAM CAMPUS city: JERUSALEM postcode: 91904 contact info Titolo: Ms. Nome: Hani Cognome: Ben-Yehuda Email: send email Telefono: +972 2 6586676 Fax: +972 722447007
Nazionalità Coordinatore	Israel [IL]
Totale costo	184˙558 €
EC contributo	184˙558 €
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	2014
Periodo (anno-mese-giorno)	2014-03-01   -   2016-02-29

 Partecipanti

#	participant	country	role	EC contrib. [€]
1	THE HEBREW UNIVERSITY OF JERUSALEM.  Organization address address: GIVAT RAM CAMPUS city: JERUSALEM postcode: 91904 contact info Titolo: Ms. Nome: Hani Cognome: Ben-Yehuda Email: send email Telefono: +972 2 6586676 Fax: +972 722447007	IL (JERUSALEM)	coordinator	184˙558.80

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 Obiettivo del progetto (Objective)

'The acceleration of high-energy particles at collisionless shocks in astrophysical plasmas is a common phenomenon in the Universe and takes place in a variety of systems, from the heliosphere up to the most distant cosmic sources. The best known example for such non-thermal particle populations are cosmic rays, but additional evidence for the existence of high energy particles comes from observations of non-thermal synchrotron and inverse Compton emission from several sources, as pulsar wind nebulae, jets from active galactic nuclei, gamma-ray bursts, and supernova remnants. In all these sources collisionless shocks are thought to be responsible for the conversion of a significant fraction of the flow energy into relativistic particles with power-law non-thermal spectra. The most popular candidate for particle energization at astrophysical shocks is the so-called diffusive shock acceleration mechanism (first-order Fermi mechanism), where charged particles gain energy by scattering back and forth between the converging upstream and downstream plasmas. In collisionless astrophysical plasmas the source of scattering is provided by magnetic turbulence rather than by Coulomb collisions. Efficient acceleration requires that particles repeatedly cross the shock. For the accelerated particles a power-law spectrum is the natural product of collisionless shock acceleration. I propose to investigate the implications of shock acceleration in gamma-ray bursts and in supernova remnants and to set constraints on the acceleration mechanism. This research project consists of two parts, one concerning the acceleration of electrons at the external shocks of gamma-ray bursts and the resulting emission, and the other one focused on the acceleration of cosmic rays at the front shock of supernova remnants and their diffusion into the Galaxy.'