SYMBIOJETS
Jets in Symbiotic Stars -- the Rosetta stone for jet formation
| Coordinatore | UNIVERSITA DEGLI STUDI DI TORINO
Organization address
address: Via Giuseppe Verdi 8 contact info |
| Nazionalità Coordinatore | Italy [IT] |
| Totale costo | 30˙000 € |
| EC contributo | 30˙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-2009-RG |
| Funding Scheme | MC-ERG |
| Anno di inizio | 2010 |
| Periodo (anno-mese-giorno) | 2010-04-01 - 2012-03-31 |
Partecipanti
| # | ||||
|---|---|---|---|---|
| 1 |
UNIVERSITA DEGLI STUDI DI TORINO
Organization address
address: Via Giuseppe Verdi 8 contact info |
IT (TORINO) | coordinator | 30˙000.00 |
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Obiettivo del progetto (Objective)
'Although jets are ubiquitous phenomena in many different astrophysical objects, their formation is still relatively unclear. We find jets in young stellar objects (YSO), in Planetary and Proto-Planetary nebulae, in Symbiotic Stars (SySs), in X-ray binaries and active galactic nuclei. The mass loss rate of all jets is found to be connected to the mass accretion rate of the underlying disk found in most objects. Hence it is believed that a single universal mechanism is responsible for ejecting jets in all classes. Since the necessary components seem to be well known and common to all objects, a more careful investigation of one specific class of objects should promise new insights also for the mechanisms in the other classes. From the observational point of view, one needs observational data with a high spatial resolution and kinematic informations from regions as near as possible to the jet source. These aspects make Symbiotic Stars as a class to ideal testbeds. Also for a theoretical reason, Symbiotic Stars are ideal for studying jet formation: their close relationship with cataclysmic variables (CVs). The short timescales in CVs make the latter the best understood accreting systems. Remarkably, although the WD in CVs may be highly magnetized, no jet emission has been detected thus far from these objects. Only hints for a present jet in one object (the dwarf nova SS Cyg) have been found very recently (Koerding et al. 2008). Even after confirmation of this result, the striking dichotomy concerning the fraction of jet sources to non-jet emitting objects in SySs (10 out of about 220) and that in CVs (one out of a few thousand) still lacks a compelling explanation. If we understand the propagating jet, we can compare it with analytical models and known relations between the properties inside the jet and those close to the disk, in order to infer basic parameters of the jet engine and to find intrinsic differences between SySs and CVs.'
Introduzione (Teaser)
Some of the most amazing objects in the Universe are the cosmic jets of plasma ejected at close to the speed of light from numerous astrophysical objects. EU-funded researchers evaluated data from a model star system that could provide information about the mechanisms of jet formation potentially shared by all objects with which they are associated.