The astrophysical jet

Le résumé fourni par la source

From the first eight chapters, we conclude that the subject of astrophysical jets has seen observational advances over the last twenty years that take it almost beyond recognition in breadth and depth. The penultimate two chapters have shown how the major theories from the 1980s have been developed and adapted but not dismissed. Yet, there are long-standing debates which have not found a resolution and new issues which stretch our understanding. The challenging themes can be listed under the following headings. We still need to gather evidence for: The process of formation and launch The collimation and acceleration The propagation, structure and stability The contents, both near and far from the driving source. Here, rather than providing a long list of questions, we focus on some specific hot issues relevant to the general subject: the composition, regulation, feedback and unification. Composition The physical parameters, such as the energy, speed, mass flux and abundances of jet material, can often be constrained after identifying the radiation process. However, invisible components, whose presence has not yet been settled, may be flowing out adjacent to the radiating material or mixed in on the particle scale. For example, in the observed warm atomic and cold molecular jets from young stars and protostars, there may be more outflowing mass in the form of cold neutral atomic gas (Nisini et al ., 2005). In addition, dust internal to the jet avoids direct detection (Dionatos et al ., 2009).

Ce résumé expose les affirmations des auteurs. BNTIC ne l’interprète pas comme une validation indépendante des résultats.