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Introduction
Published in Kurt A. Polzin, Ashley K. Hallock, Kamesh Sankaran, Justin M. Little, Circuit Modeling of Inductively-Coupled Pulsed Accelerators, 2023
Kurt A. Polzin, Ashley K. Hallock, Kamesh Sankaran, Justin M. Little
Inductive pulsed plasma accelerators [1] are typically categorized by the nature of their magnetic flux lines. While all magnetic flux lines close on themselves, the term “open” magnetic flux in this case refers to a configuration where the currents in the external driving circuit coil and the plasma produce a concentrated axisymmetric r-z magnetic field sandwiched between the two currents. This can be accomplished either in the planar configuration shown in Fig. 1.2a, producing an axially-accelerating plasma sheet, or in the conical theta-pinch configuration shown in Fig. 1.2b, yielding a plasma sheet that is accelerated both in the radially-inward and axial directions. In contrast to either of those devices, the plasma in a third design permutation known as the theta-pinch is inductively squeezed in a pure radially-inward direction. In any of these configurations the concentrated field lines in the r-z plane, once leaving the space between the external coil and the plasma, expand to fill space until they reconnect to themselves on the other side of the external coil as illustrated in Fig.1.3.
Sources of UV Light
Published in Tatiana Koutchma, Ultraviolet Light in Food Technology, 2019
The Surface Discharge (SD) lamp developed by Phoenix Science & Technology Inc. (Chelmsford, MA) is a PUV lamp that overcomes the disadvantages of flash lamps. According to Schaefer et al. (2007), a high-power electrical pulse is discharged along the surface of a dielectric tube and generates a uniform plasma sheet along the substrate tube, producing an intense light pulse. The intensity and efficiency of the pulsed UV lamp is much greater than that of traditional mercury low- and medium-pressure lamps and commercially available pulsed flash lamps. The discharge is in a rare gas (xenon or krypton) that is non-toxic. The envelope serves only as a container for the rare gas and plays no role in the discharge (Figure 2.11).
Study of space plasma waves with flow
Published in Radiation Effects and Defects in Solids, 2022
T. Smith, K. Strong, S. Ibenki, S. Sen
Similarly, large plasma fluid flows are also a hallmark of the Earth’s magnetosphere, magnetotail and plasma sheet. It has been recognized in early substorm research that high-speed plasma flows occur during substorms. In the plasmasphere, steep shear in ion flow velocity can exist due to the dominating co-rotating electric field inside the plasmasphere and a convective magnetospheric electric field penetrating across the plasmapause (4). Also, there are a number of observational confirmations of the presence of a variety of plasma flows in the upper levels of the solar atmosphere (spicules and macrospicules, reconnection outflows, jets in coronal holes, etc). Often, the plasma flows are directed along the magnetic field and are compact in the transversal direction. Note that the inhomogeneous flows do not always coincide with the inhomogeneities in the plasma density and magnetic field. Moreover, even in a homogeneous plasma there can be inhomogeneous flows, corresponding to the shifting of one plasma layer relative to another, along the magnetic field (5). Also, the boundaries between the fast and slow streams of the solar wind flow is also sheared.
Non-uniform flow in plasma
Published in Radiation Effects and Defects in Solids, 2020
T. Smith, I. Mombo, M. Rhinehart, P. Adegbaye, S. Ebenki, C. Standfield, S. Sen
Similarly large plasma fluid flows are also a hallmark of the Earth's magnetosphere, magnetotail and plasma sheet. It has been recognized in early substorm research that high-speed plasma flows occur during substorms. In the plasmasphere, steep shear in ion flow velocity can exist due to the dominating co-rotating electric field inside the plasmasphre and a convective magnetospheric electric field penetrating across the plasmapause (4). Also there are a number of observational confirmations of the presence of a variety of plasma flows in the upper levels of the solar atmosphere (spicules and macrospicules, reconnection outflows, jets in coronal holes, etc). Often, the plasma flows are directed along the magnetic field and are compact in the transversal direction. Note that the inhomogeneous flows do not always coincide with the inhomogeneities in the plasma density and magnetic field. Moreover, even in a homogeneous plasma there can be inhomogeneous flows, corresponding to the shifting of one plasma layer relative to another, along the magnetic field (5). Also the boundaries between the fast and slow streams of the solar wind flow is also sheared.