CURRENT SHEETS EQUIVALENT TO END WINDING CURRENTS OF INDUCTION MOTOR ROTOR AND DETERMINATION OF THE MAGNETIC FIELD IN THE END ZONE. Part II. Flux densities due to rotor end winding

An analysis of the induction equation shows that the level surfaces of the magnetic field in a resistive plasma satisfy a certain bound upon the time means of their areas. When this bound is applied to some configurations typical of chaotic plasmas, it is shown that the number of bidimensional sheets where the field reaches a extremum is bounded, whereas the number of extremal ropes or points need not be. This also applies to current sheets.

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Transport of energetic particles from reconnecting current sheets in flaring corona to the heliosphere

10.5194/egusphere-egu21-15163 ◽

2021 ◽

Author(s):

Philippa Browning ◽

Mykola Gordovskyy ◽

Satashi Inoue ◽

Eduard Kontar ◽

Kanya Kusano ◽

...

Keyword(s):

Magnetic Field ◽

Energetic Particles ◽

Transport Processes ◽

Data Driven ◽

Current Sheets ◽

Electrons And Ions ◽

Data Driven Approach ◽

Particle Simulations ◽

The Magnetic Field

In this study, we inverstigate the acceleration of electrons and ions at current sheets in the flaring solar corona, and their transport into the heliosphere. We consider both generic solar flare models and specific flaring events with a data-driven approach. The aim is to answer two questions: (a) what fraction of particles accelerated in different flares can escape into the heliosphere?; and (b) what are the characteristics of the particle populations propagating towards the chromosphere and into the heliosphere?We use a combination of data-driven 3D magnetohydrodynamics simulations with drift-kinetic particle simulations to model the evolution of the magnetic field and both thermal and non-thermal plasma and to forward-model observable characteristics. Particles are accelerated in current sheets associated with flaring reconnection. When applied to a specific flare, the model successfully predicts observed features such as the location and relative intensity of hard X-ray sources and helioseismic source locations. This confirms the viability of the approach.Using these MHD-particle models, we will show how the magnetic field evolution and particle transport processes affect the characteristics of both energetic electrons and ions in the the inner corona and the heliosphere. The implications for interpretation of in situ measurements of energetic particles by Solar Orbiter and Parker Solar Probe will be discussed.&#160;&#160;

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Zum Rotations-Zeeman-Effekt in Dimethylketen / Molecular Zeeman Effect and the Determination of the Molecular g Values, Paramagnetic Susceptibilities, and Molecular Quadrupole Moments in Dimethylketene

Zeitschrift für Naturforschung A ◽

10.1515/zna-1972-0409 ◽

1972 ◽

Vol 27 (4) ◽

pp. 597-600 ◽

Cited By ~ 2

Author(s):

D. Sutter ◽

L. Charpentier ◽

H. Dreizler

Keyword(s):

Magnetic Field ◽

Zeeman Effect ◽

Microwave Spectrum ◽

Quadrupole Moments ◽

Selection Rules ◽

Rotational Transitions ◽

The Magnetic Field

Abstract The rotational Zeeman-Effect in the microwave spectrum of dimethylketene was investigated at fieldstrengths close to 22 kG. Only ΔJ= 1 rotational transitions with ΔM = ± 1 selection rules did show appreciable splittings due to the magnetic field. From the splittings the diagonal elements of the molecular gr-tensor were determined to be: gaa = ∓ 0.020(3) ; gbb = ∓ 0.0165(8) ; gcc= + 0.0126(5). (Only the relative signs of the g-values are obtained from the experiment). The susceptibility anisotropics were found to be close to zero.

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