Direct evidence for the presence of an inertial energy cascade, the most characteristic signature of hydromagnetic turbulence (MHD), is observed in the solar wind by the Ulysses spacecraft. After a brief rederivation of the equivalent of Yaglom's law for MHD turbulence, a linear relation is indeed observed for the scaling of mixed third-order structure functions involving Elsässer variables. Th...

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This paper investigates the steady hydromagnetic three-dimensional boundary layer flow of Maxwell fluid over a bidirectional stretching surface. Both cases of prescribed surface temperature (PST) and prescribed surface heat flux (PHF) are considered. Computations are made for the velocities and temperatures. Results are plotted and analyzed for PST and PHF cases. Convergence analysis is present...

Title of dissertation: HYDROMAGNETIC TURBULENT INSTABILITY IN LIQUID SODIUM EXPERIMENTS Daniel R. Sisan, Doctor of Philosophy, 2004 Dissertation directed by: Professor Daniel P. Lathrop Department of Physics This dissertation describes the observation of magnetically-induced instabilities that occur from a preexisting hydrodynamically turbulent background. We claim these instabilities are the f...

Time-dependent hydromagnetic phenomena in a rotating spherical cavity are investigated in the framework of an interior boundary-layer expansion. The interior problem is shown to contain waves whose frequencies are of order o, A o and A2u, where w is the rotation rate of the cavity and A2 = B2/4npu2R2 < 1 is the Alfven number. B is an imposed magnetic field, p the fluid density and R the radius ...

Evidence accumulated over the past several decades indicates that a large-scale applied (dc) magnetic field imposes a preferred direction on turbulence, and thus plays an important role in plasma diffusion [1], energetic particle scattering [2], and plasma heating [3–5]. Each of these in turn may significantly influence large-scale flows and structure [6–8]. The interplay between turbulence and...

The stability properties of newly born neutron stars, or proto–neutron stars (PNSs), are considered. We take into account dissipative processes, such as neutrino transport and viscosity, in the presence of a magnetic field. In order to find the regions of the star subject to different sorts of instability, we derive the general instability criteria and apply it to evolutionary models of PNSs. T...

We study the stability of compressible differentially rotating flows in the presence of the magnetic field, and we show that the compressibility profoundly alters the previous results for a magnetized incompressible flow. The necessary condition of newly found instability can be easily satisfied in various flows in laboratory and astrophysical conditions and reads BsBphiOmega' not equal to 0, w...

Es werden Wellen in einem quasi-neutralen Gas untersucht, das Ionen und Elektronen enthält und genügend kalt ist, so daß die thermischen Bewegungen vernachlässigt werden können. Außerdem werden Zusammenstöße zwischen den Teilchen vernachlässigt, jedoch nicht die Trägheitseffekte des elektrischen Stromes. Die nicht-linearen Gleichungen für unendlich ausgedehnte, ebene Kompressionswellen, die sic...