Astrophysical Jets and Outflows

Elisabete M. de Gouveia Dal Pino

doi:10.1016/j.asr.2005.03.145

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arXiv · astro-ph/0406319

Astrophysical Jets and Outflows

Elisabete M. de Gouveia Dal Pino

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Abstract

Highly collimated supersonic jets and less collimated outflows are observed to emerge from a wide variety of astrophysical objects. They are seen in young stellar objects (YSOs), proto-planetary nebulae, compact objects (like galactic black holes or microquasars, and X-ray binary stars), and in the nuclei of active galaxies (AGNs). Despite their different physical scales (in size, velocity, and amount of energy transported), they have strong morphological similarities. What physics do they share? These systems either hydrodynamic or magnetohydrodynamic (MHD) in nature and are, as such, governed by non-linear equations. While theoretical models helped us to understand the basic physics of these objects, numerical simulations have been allowing us to go beyond the one-dimensional, steady-state approach extracting vital information. In this lecture, the formation, structure, and evolution of the jets are reviewed with the help of observational information, MHD and purely hydrodynamical modeling, and numerical simulations. Possible applications of the models particularly to YSOs and AGN jets are addressed.

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Elisabete M. de Gouveia Dal Pino. 2004-06-14. Astrophysical Jets and Outflows. https://doi.org/10.1016/j.asr.2005.03.145

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