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Published byLogan Shaddix Modified over 2 years ago

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ANALYTICAL STUDIES OF MHD OUTFLOWS Self-similar solutions Outflows from stellar bodies From Solar Wind To Stellar winds (O M stars) Compact objects (pulsars, …) AGN GRB From 1-D Hydro steady model (Parker 1958) To 3-D MHD relativistic time dep. codes Collimated flows: Steady and axisymmetric MHD approach

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Blandford & Payne ‘82, ……

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Low & Tsinganos ‘85, Sauty et al. ’94, …….

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> 0 < 0

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Weak collim. in relat. outflows time dependent computations ( Tsinganos & Bogovalov, ) Possible Model: Inner relativistic wind Outer classical disk wind

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CONCLUSIONS Through the analysis of MHD steady solutions we can have insights on the physical properties of astrophysical outflows Further issues: Non ideal MHD (resistivity) Radiative effects (losses and/or acceleration) Large amplitute e.m. waves Time dependent solutions: Asympt. status, instabilities Interaction with the envir. Launch …….

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