scholarly journals Role of magnetic flux expulsion to reach Q0>3×1010 in superconducting rf cryomodules

2019 ◽  
Vol 22 (3) ◽  
Author(s):  
S. Posen ◽  
G. Wu ◽  
A. Grassellino ◽  
E. Harms ◽  
O. S. Melnychuk ◽  
...  
Keyword(s):  
Magnetic Flux ◽  
Superconducting Rf ◽  
Flux Expulsion

scholarly journals Magneto-optical spectroscopy of highly aligned carbon nanotubes: Identifying the role of threading magnetic flux

2008 ◽  
Vol 78 (8) ◽  
Author(s):  
J. Shaver ◽  
S. A. Crooker ◽  
J. A. Fagan ◽  
E. K. Hobbie ◽  
N. Ubrig ◽  
...  
Keyword(s):  
Carbon Nanotubes ◽  
Magnetic Flux ◽  
Optical Spectroscopy ◽  
Aligned Carbon Nanotubes

scholarly journals Processes and mechanisms governing the initiation and propagation of CMEs

2008 ◽  
Vol 26 (10) ◽  
pp. 3089-3101 ◽  
Author(s):  
B. Vršnak
Keyword(s):  
Magnetic Flux ◽  
External Disturbance ◽  
Source Region ◽  
Flux Rope ◽  
Impulsive Phase ◽  
3 Dimensional ◽  
Initiation And Propagation ◽  
Region Size ◽  
The Magnetic Field

Abstract. The most important observational characteristics of coronal mass ejections (CMEs) are summarized, emphasizing those aspects which are relevant for testing physical concepts employed to explain the CME take-off and propagation. In particular, the kinematics, scalings, and the CME-flare relationship are stressed. Special attention is paid to 3-dimensional (3-D) topology of the magnetic field structures, particularly to aspects related to the concept of semi-toroidal flux-rope anchored at both ends in the dense photosphere and embedded in the coronal magnetic arcade. Observations are compared with physical principles and concepts employed in explaining the CME phenomenon, and implications are discussed. A simple flux-rope model is used to explain various stages of the eruption. The model is able to reproduce all basic observational requirements: stable equilibrium and possible oscillations around equilibrium, metastable state and possible destabilization by an external disturbance, pre-eruptive gradual-rise until loss of equilibrium, possibility of fallback events and failed eruptions, relationship between impulsiveness of the CME acceleration and the source-region size, etc. However, it is shown that the purely ideal MHD process cannot account for highest observed accelerations which can attain values up to 10 km s−2. Such accelerations can be achieved if the process of reconnection beneath the erupting flux-rope is included into the model. Essentially, the role of reconnection is in changing the magnetic flux associated with the flux-rope current and supplying "fresh" poloidal magnetic flux to the rope. These effects help sustain the electric current flowing along the flux-rope, and consequently, reinforce and prolong the CME acceleration. The model straightforwardly explains the observed synchronization of the flare impulsive phase and the CME main-acceleration stage, as well as the correlations between various CME and flare parameters.

Control of magnetic flux and eddy currents in magnetic films for on-chip radio frequency inductors: Role of the magnetic vias

2014 ◽  
Vol 115 (17) ◽  
pp. 17E719 ◽  
Author(s):  
Hao Wu ◽  
Donald S. Gardner ◽  
Shirong Zhao ◽  
Hai Huang ◽  
Hongbin Yu
Keyword(s):  
Magnetic Flux ◽  
Radio Frequency ◽  
Eddy Currents ◽  
Magnetic Films ◽  
On Chip

scholarly journals Turbulence and dynamo interlinks

2012 ◽  
Vol 8 (S294) ◽  
pp. 337-348
Author(s):  
E. M. de Gouveia Dal Pino ◽  
R. Santos-Lima ◽  
G. Kowal ◽  
D. Falceta-Gonçalves
Keyword(s):  
Magnetic Fields ◽  
Magnetic Flux ◽  
Magnetic Reconnection ◽  
Small Scale ◽  
Low Density ◽  
Mhd Turbulence ◽  
Turbulent Dynamo ◽  
Dynamo Process

AbstractThe role of turbulence in astrophysical environments and its interplay with magnetic fields is still highly debated. In this lecture, we will discuss this issue in the framework of dynamo processes. We will first present a very brief summary of turbulent dynamo theories, then will focus on small scale turbulent dynamos and their particular relevance on the origin and maintenance of magnetic fields in the intra-cluster media (ICM) of galaxies. In these environments, the very low density of the flow requires a collisionless-MHD treatment. We will show the implications of this approach in the turbulent amplification of the magnetic fields in these environments. To finalize, we will also briefly address the connection between MHD turbulence and fast magnetic reconnection and its possible implications in the diffusion of magnetic flux in the dynamo process.

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