Abstract
We present the MHD simulation including accretion flows in disks, acceleration of outflows from disks, and collimation of the outflows self-consistently. Although it was considered that this kind of simulations only shows the transient phenomena of jets, we found that the outflow and accretion flow reached a quasi-steady state by performing a long-term calculation in a large calculation region. Though the final stage is not exactly the steady state, the acceleration and collimation mechanisms of the outflow were the same as those of the steady theory. The scale of the calculation is approaching to the scale that was observed by the VLBI technique, which provides the current highest resolution for YSO jets.
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© 2003 Springer Science+Business Media Dordrecht
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Kudoh, T., Matsumoto, R., Shibata, K. (2003). Mhd Simulations of Jets From Accretion Disks. 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_16
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DOI: https://doi.org/10.1007/978-94-007-0999-7_16
Publisher Name: Springer, Dordrecht
Print ISBN: 978-94-010-3764-8
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