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Outflows from young stars : The Rosetta stone of astrophysicalJets?

Published online by Cambridge University Press:  13 February 2013

T. Ray
T. Ray*
Affiliation:
School of Cosmic Physics, Dublin Institute for Advanced Studies, 31 Fitzwilliam Place, Dublin 2, Ireland

Abstract

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It can be argued that all astrophysical jets, from lowly sub-stellar objects such asyoung brown dwarfs to massive black holes at the centre of AGN, are generated by the samebasic physical mechanism. While the nature of that mechanism is still debated, jets fromyoung stars may represent our best chance of deciphering it. There are several reasons forthis statement. First of all they are nearby, thus affording us not only high spatialresolution studies of the “central engine” but also time-resolved analysis of theirkinematics. Moreover as they radiate emission lines, spectroscopy can reveal radialvelocities, temperature, density, ion fraction, etc., along their flow. This wealth ofdata is a challenge to the theorist/computational simulator but also a highly effectivemeans of discriminating between models. In addition, the observations tightly constrainlaboratory experiments. Here, I briefly review what is known about conditions in jets fromyoung stars as a guide to experiments, their generation including their link withaccretion disks, and their evolution from the earliest proto-stellar to pre-main sequencephase.

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