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Jets From Young Stars III - Numerical MHD and Instabilities (Hardcover, 2008 ed.)
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Jets From Young Stars III - Numerical MHD and Instabilities (Hardcover, 2008 ed.)
Series: Lecture Notes in Physics, 754
Expected to ship within 10 - 15 working days
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The study of the mechanisms that govern origin and propagation of
stellar jets involves the treatment of many concurrent physical
processes such as gravitation, hydrodynamics and
magnetohydrodynamics, atomic physics and radiation. In the past
years, an intensive work has been done looking for so- tions of the
ideal MHD equations in the steady state limit as well as studying
the stability of out?ows in the linear regime. These kind, of
approaches have provided a contribution to the understanding of
jets that can hardly be ov- estimated. However, the extension of
the analyses to the time-dependent and nonlinear regimes could not
be avoided, and the MHD numerical simulations were the only mean to
achieve this goal.
Intherecentyears,considerableprogresseshavebeenmadebythecom-
tational?uiddynamiccommunityinthedevelopmentofnumericaltechniques,
theso-calledhighresolutionshockcapturingschemes,wellsuitedforthetre-
ment of supersonic ?ows with discontinuities. The numerical
simulations of astrophysical jets took advantage of these
developments; however new physics needed to be incorporated, such
as magnetic ?eld e?ects, radiation losses by diluted gases, and
proper astrophysics environments. These needs led to the nontrivial
extension of the methods devised for the Euler equations of g-
dynamics to the magneto-hydrodynamical system. On the other hand,
the possibility of carrying out numerical calculations has been
greatly facilitated bytheavailability,
ononehand,ofpowerfulsupercomputersand,ontheother hand, of fast
processors at low cost. Large scale 3D simulations of jets at high
resolution are now possible thanks to supercomputers, but also high
reso- tion 2D MHD simulations can be performed routinely on desktop
computers.
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