ACCURATE MAGNETIC FLUX MEASUREMENTS IN ELECTROMAGNETIC RAIL LAUNCHERS

2013 ◽  
Vol 40 ◽  
pp. 243-256
Author(s):  
Roberto Ferrero ◽  
Mirko Marracci ◽  
Bernardo Tellini
Keyword(s):  
Magnetic Flux ◽  
Flux Measurements ◽  
Electromagnetic Rail Launchers

1428 Evaluation of process tribology by three dimensional residual magnetic flux measurements

2008 ◽  
Vol 2008.1 (0) ◽  
pp. 263-264
Author(s):  
Sadao KUWADURU ◽  
Syuuichi TUKAHARA ◽  
Takuma TOJO ◽  
Shigeo KOTAKE ◽  
Yasuyuki SUZUKI
Keyword(s):  
Magnetic Flux ◽  
Three Dimensional ◽  
Flux Measurements

Evaluation of a Linear Hybrid Microstep Motor by Means of Magnetic Flux Measurements

2007 ◽  
Vol 43 (6) ◽  
pp. 2588-2590 ◽  
Author(s):  
M. Hahn ◽  
M. Bedenbecker ◽  
H. H. Gatzen
Keyword(s):  
Magnetic Flux ◽  
Flux Measurements

scholarly journals Integrator Drift Compensation of Magnetic Flux Transducers by Feed-Forward Correction

Sensors ◽  
2019 ◽  
Vol 19 (24) ◽  
pp. 5455 ◽  
Author(s):  
Maria Amodeo ◽  
Pasquale Arpaia ◽  
Marco Buzio
Keyword(s):  
Magnetic Flux ◽  
State Of The Art ◽  
Proton Synchrotron ◽  
Particle Accelerators ◽  
Magnetic Cycle ◽  
Short Term ◽  
Feed Forward ◽  
Flux Measurements ◽  
Drift Compensation

Integrator drift is a problem strongly felt in different measurement fields, often detrimental even for short-term applications. An analytical method for modelling and feed-forward correcting drift in magnetic flux measurements was developed analytically and tested experimentally. A case study is reported on the proof of principle as a novel kind of quasi-DC field marker of the 5-ppm Nuclear Magnetic Resonance (NMR) transducer Metrolab PT2026, applied to the Extra Low ENergy Antiproton (ELENA) ring and the Proton Synchrotron Booster (PSB) at CERN. In some particle accelerators, such as in ELENA, the resulting feed-forward correction guarantees 1 μ T field stability over 120-s long magnetic cycle on a plateau of 50 mT, reducing by three orders of magnitude the field error caused by the integrator drift with respect to the state of the art.

Simple and Inexpensive Test Equipment for Magnetic Flux Measurements in a Ferromagnetic Core

1980 ◽  
Vol 17 (4) ◽  
pp. 301-307
Author(s):  
Arifur Rahman
Keyword(s):  
Magnetic Flux ◽  
Laboratory Test ◽  
Magnetization Curve ◽  
Magnetic Circuit ◽  
Test Equipment ◽  
Test Results ◽  
Ferromagnetic Core ◽  
Flux Measurements ◽  
Normal Magnetization

This paper describes a simple laboratory test equipment for classroom determination of the normal magnetization curve and hysteresis loop of a built-in ferromagnetic core. The circuit details, steps of design of the magnetic circuit coils and test results are also presented.

Needle-probe techniques for local magnetic flux measurements

2003 ◽  
Vol 93 (10) ◽  
pp. 8271-8273 ◽  
Author(s):  
Marc De Wulf ◽  
Luc Dupré ◽  
Dimitre Makaveev ◽  
Jan Melkebeek
Keyword(s):  
Magnetic Flux ◽  
Needle Probe ◽  
Flux Measurements

Emergence of Twisted Magnetic Flux Related Sigmoidal Brightening

2000 ◽  
Vol 179 ◽  
pp. 263-264
Author(s):  
K. Sundara Raman ◽  
K. B. Ramesh ◽  
R. Selvendran ◽  
P. S. M. Aleem ◽  
K. M. Hiremath
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Magnetic Flux ◽  
Ultra Violet ◽  
Active Regions ◽  
Morphological Properties ◽  
Energy Storage And Conversion ◽  
The Sun ◽  
X Rays ◽  
The Magnetic Field

Extended AbstractWe have examined the morphological properties of a sigmoid associated with an SXR (soft X-ray) flare. The sigmoid is cospatial with the EUV (extreme ultra violet) images and in the optical part lies along an S-shaped Hαfilament. The photoheliogram shows flux emergence within an existingδtype sunspot which has caused the rotation of the umbrae giving rise to the sigmoidal brightening.It is now widely accepted that flares derive their energy from the magnetic fields of the active regions and coronal levels are considered to be the flare sites. But still a satisfactory understanding of the flare processes has not been achieved because of the difficulties encountered to predict and estimate the probability of flare eruptions. The convection flows and vortices below the photosphere transport and concentrate magnetic field, which subsequently appear as active regions in the photosphere (Rust & Kumar 1994 and the references therein). Successive emergence of magnetic flux, twist the field, creating flare productive magnetic shear and has been studied by many authors (Sundara Ramanet al.1998 and the references therein). Hence, it is considered that the flare is powered by the energy stored in the twisted magnetic flux tubes (Kurokawa 1996 and the references therein). Rust & Kumar (1996) named the S-shaped bright coronal loops that appear in soft X-rays as ‘Sigmoids’ and concluded that this S-shaped distortion is due to the twist developed in the magnetic field lines. These transient sigmoidal features tell a great deal about unstable coronal magnetic fields, as these regions are more likely to be eruptive (Canfieldet al.1999). As the magnetic fields of the active regions are deep rooted in the Sun, the twist developed in the subphotospheric flux tube penetrates the photosphere and extends in to the corona. Thus, it is essentially favourable for the subphotospheric twist to unwind the twist and transmit it through the photosphere to the corona. Therefore, it becomes essential to make complete observational descriptions of a flare from the magnetic field changes that are taking place in different atmospheric levels of the Sun, to pin down the energy storage and conversion process that trigger the flare phenomena.

Large-scale Motion of Solar Filaments

2000 ◽  
Vol 179 ◽  
pp. 205-208
Author(s):  
Pavel Ambrož ◽  
Alfred Schroll
Keyword(s):  
Magnetic Flux ◽  
Proper Motion ◽  
Time Scale ◽  
Large Scale ◽  
Accuracy Of Measurements ◽  
Solar Filaments ◽  
General Movement ◽  
Scale Motion ◽  
Velocity Scatter

AbstractPrecise measurements of heliographic position of solar filaments were used for determination of the proper motion of solar filaments on the time-scale of days. The filaments have a tendency to make a shaking or waving of the external structure and to make a general movement of whole filament body, coinciding with the transport of the magnetic flux in the photosphere. The velocity scatter of individual measured points is about one order higher than the accuracy of measurements.

Solar Filaments as Tracers of Subsurface Processes

2000 ◽  
Vol 179 ◽  
pp. 177-183
Author(s):  
D. M. Rust
Keyword(s):  
Magnetic Fields ◽  
Magnetic Flux ◽  
Coronal Mass Ejections ◽  
Interplanetary Space ◽  
Intermediate Stage ◽  
Coronal Plasma ◽  
Magnetic Helicity ◽  
The Sun ◽  
New Paradigm ◽  
Solar Filaments

AbstractSolar filaments are discussed in terms of two contrasting paradigms. The standard paradigm is that filaments are formed by condensation of coronal plasma into magnetic fields that are twisted or dimpled as a consequence of motions of the fields’ sources in the photosphere. According to a new paradigm, filaments form in rising, twisted flux ropes and are a necessary intermediate stage in the transfer to interplanetary space of dynamo-generated magnetic flux. It is argued that the accumulation of magnetic helicity in filaments and their coronal surroundings leads to filament eruptions and coronal mass ejections. These ejections relieve the Sun of the flux generated by the dynamo and make way for the flux of the next cycle.

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