Abstract
By using relativistic, axisymmetric, ideal MHD, we examine the motion of the baryon/e±/ photon fluid that emanates from a stellar-mass compact object/debris-disk system (a common outcome of many progenitor models). We prove that the motion can be described as a frozen pulse, which permits the study of each shell of the pancake-shaped outflow using steady-state equations. The ejected energy flux is dominated by the electromagnetic (Poynting) contribution, but it can also have a nonnegligible e±;/radiation (thermal fireball) component. We demonstrate, through exact selfsimilar solutions, that the flow is first thermally and subsequently magnetically accelerated up to equipartition between kinetic and Poynting fluxes, i.e., ∼ 50% of the total energy is converted into baryonic kinetic energy. The electromagnetic forces also collimate the flow, reaching a cylindrical structure asymptotically.
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© 2003 Springer Science+Business Media Dordrecht
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Vlahakis, N., KÖNigl, A. (2003). A Model for Grb Jets. In: Fernandes, A.J.L., Garcia, P.J.V., Lima, J.J.G. (eds) Jets in Young Stellar Objects. Springer, Dordrecht. https://doi.org/10.1007/978-94-007-0999-7_41
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DOI: https://doi.org/10.1007/978-94-007-0999-7_41
Publisher Name: Springer, Dordrecht
Print ISBN: 978-94-010-3764-8
Online ISBN: 978-94-007-0999-7
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