scholarly journals North-South Asymmetry of the Interplanetary Magnetic Field Magnitude and the Geomagnetic Indices

2016 ◽  
Vol 06 (01) ◽  
pp. 14-22 ◽  
Author(s):  
Mohammed Ali El-Borie ◽  
Ali Abdel-Moniem Abdel-Halim ◽  
Shady Yousry El-Monier
Keyword(s):  
Magnetic Field ◽  
Interplanetary Magnetic Field ◽  
Field Magnitude ◽  
Geomagnetic Indices ◽  
Magnetic Field Magnitude ◽  
South Asymmetry

Solar wind and bow shock parameters affecting turbulence development inside the magnetosheath

2021 ◽  
Author(s):  
Liudmila Rakhmanova ◽  
Maria Riazantseva ◽  
Georgy Zastenker ◽  
Yuri Yermolaev
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Interplanetary Magnetic Field ◽  
Bow Shock ◽  
Mutual Orientation ◽  
Frequency Spectra ◽  
Field Magnitude ◽  
Magnetic Field Magnitude ◽  
Solar Wind Parameters ◽  
Turbulent Cascade

<p>Development of the turbulent cascade inside the magnetosheath is known to be affected by the bow shock. Recently a number of studies showed various scenario of turbulent cascade modification at the bow shock including deviation from Kolmogorov scaling and additional damping of the kinetic-scale compressive fluctuations. Also, properties of probability distribution function may be modified behind the bow shock. However, factors which govern turbulence development in the magnetosheath remain unclear. Present study focuses on experimental analysis of the solar wind parameters which influence turbulence inside the magnetosheath. Analyzed data involves the combination of the solar wind parameters measured in L1 point by WIND spacecraft and Themis, Cluster and Spektr-R measurements behind the bow shock. Parameters of the frequency spectra of ion flux and/or magnetic field magnitude at frequency band from 0.01 to 2-10 Hz are considered such as slopes at magnetohydrodynamic and kinetic scales and the break frequency. Parameters of spectra are considered behind the bow shock of various topology i.e. for different mutual orientation of the interplanetary magnetic field and the local bow shock normal. Also, distance from the analyzed point to the bow shock nose is taken to the account. Obtained results point out that modification of the turbulent cascade at the bow shock is controlled not only by the bow shock topology but also by variability of the upstream solar wind plasma parameters and direction of the interplanetary magnetic field. In particular, Kolmogorov scaling often survives across the bow shock during periods of high-amplitude variations of plasma density and magnetic field magnitude in the solar wind. Also, increasing amplitude of northern interplanetary magnetic field results in steepening of spectra behind the bow shock.  </p>

Influence of Heating Temperature on the ΔЕ-Effect of Amorphous Fe75Si10B15 Wires

2014 ◽  
Vol 215 ◽  
pp. 264-267
Author(s):  
Andrey Semenov ◽  
Evgeniy Golygin ◽  
Alexey Gavriliuk ◽  
Alexander Mokhovikov ◽  
Alexander Gafarov ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Inner Core ◽  
Heating Temperature ◽  
Amorphous Wire ◽  
Absolute Value ◽  
Tensile Stresses ◽  
Magnetoelastic Coupling ◽  
Field Magnitude ◽  
Magnetic Field Magnitude ◽  
Dc Current

In the present work we have investigated the influence of the thermocycling on the magnetoelastic parameters (the ΔЕ-effect) of amorphous Fe75Si10B15 wires, which had been pretreated by dc current j with simultaneous applying of the tensile stresses σ. It was figured out the ΔЕ-effect behavior depends strongly on pretreatment circumstances. Namely, we have got the maximum absolute value of the ΔЕ-effect shifted into direction of the higher magnetic field magnitude at j<39 MA/m2 and σ<127 MPa. In addition, the negative ΔЕ-effect was not observed for samples, pretreated at j≥45MА/m2 or σ≥128 MPa . The features of such a behavior of the ΔЕ-effect were explained in terms of the magnetoelastic coupling between the inner core and the outer shell of the amorphous wire.

scholarly journals New Force-Free Models of Magnetic Clouds

2005 ◽  
Vol 13 ◽  
pp. 133-133
Author(s):  
M. Vandas ◽  
E. P. Romashets ◽  
S. Watari
Keyword(s):  
Magnetic Field ◽  
Magnetic Cloud ◽  
Free Field ◽  
Flux Rope ◽  
Field Vector ◽  
Magnetic Clouds ◽  
Field Magnitude ◽  
Flux Ropes ◽  
Magnetic Field Magnitude ◽  
The Magnetic Field

AbstractMagnetic clouds are thought to be large flux ropes propagating through the heliosphere. Their twisted magnetic fields are mostly modeled by a constant-alpha force-free field in a circular cylindrical flux rope (the Lundquist solution). However, the interplanetary flux ropes are three dimensional objects. In reality they possibly have a curved shape and an oblate cross section. Recently we have found two force-free models of flux ropes which takes into account the mentioned features. These are (i) a constant-alpha force-free configuration in an elliptic flux rope (Vandas & Romashets 2003, A&A, 398, 801), and (ii) a non-constant-alpha force-free field in a toroid with arbitrary aspect ratio (Romashets & Vandas 2003, AIP Conf Ser. 679, 180). Two magnetic cloud observations were analyzed. The magnetic cloud of October 18-19, 1995 has been fitted by Lepping et al. (1997, JGR, 102, 14049) with use of the Lundquist solution. The cloud has a very flat magnetic field magnitude profile. We fitted it by the elliptic solution (i). The magnetic cloud of November 17-18, 1975 has been fitted by Marubashi (1997) with use of a toroidally adjusted Lundquist solution. The cloud has a large magnetic field vector rotation and a large magnetic field magnitude increase over the background level. We fitted it by the toroidal solution (ii). The both fits match the rotation of the magnetic field vector in a comparable quality to the former fits, but the description of the magnetic field magnitude profiles is remarkable better. It is possible to incorporate temporal effects (expansion) of magnetic clouds into the new solutions through a time-dependent alpha parameter as in Shimazu & Vandas (2002, EP&S, 54, 783).

scholarly journals Magnetic Field Magnitude Modification for a Force-free Magnetic Cloud Model

Solar Physics ◽  
2018 ◽  
Vol 293 (12) ◽  
Author(s):  
R. P. Lepping ◽  
C.-C. Wu ◽  
D. B. Berdichevsky ◽  
C. Kay
Keyword(s):  
Magnetic Field ◽  
Magnetic Cloud ◽  
Cloud Model ◽  
Field Magnitude ◽  
Magnetic Field Magnitude
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