Astronomy and Astrophysics – Astrophysics
Scientific paper
Aug 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007jena.confr..51a&link_type=abstract
"JENAM-2007, "Our non-stable Universe", held 20-25 August 2007 in Yerevan, Armenia. Abstract book, p. 51-51"
Astronomy and Astrophysics
Astrophysics
Scientific paper
Astrophysical jets are physical conduits along which mass, momentum, energy are channeled from stellar, galactic and extragalactic objects to the outer medium. Geometrically, these jets are narrow conical or semi-cylindrical protrusions [1, 2]. Jets are a ubiquitous phenomenon in the universe. They span a large range of luminosity and degree of collimation, from the most powerful examples observed to emerge from the nuclei of active galaxies (or AGNs) to the jets associated to low-mass young stellar objects (YSOs) within Galaxy. In the intermediate scales between these two extremes one finds evidence of outflows associated to neutron stars, massive X-ray binary systems (with SS433 being the best example of this class), symbiotic stars, and galactic stellar mass black holes. Less collimated supersonic outflows are often observed to emerge from massive hot stars in their late stages of stellar evolution, like the luminous-blue-variable stars and also from low mass stars in the late stages, like the proto-planetary nebulae [3, 4].The jet phenomenon is seen on scales that cover more than seven orders of magnitude. Nonetheless, all the jet classes share common properties. In general, they: (i) are highly collimated and in most cases two-sided; (ii) originate in compact objects; (iii) show a chain of more or less regularly spaced emission knots which in some cases move at high speeds away from the central source; (iv) often terminate in emission lobes (with line emission in the case of the YSOs and synchrotron continuum emission in the case of the AGN jets), which are believed to be the “working surfaces” where the jets shock against the ambient medium; and (vi) show evidence of accretion of matter onto the central source via an accretion disk. In this work I present the jet phenomenon as a result of reaction of interstellar matter on the ejection of superdense relativistic blobs of matter from the central object (AGN, or YSO).
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