scholarly journals Mathematical Analysis of the 08 May 2014 Weak Storm

2021 ◽  
Vol 2021 ◽  
pp. 1-12
Author(s):  
Kevser Köklü
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Mathematical Models ◽  
Mathematical Analysis ◽  
Time Scale ◽  
Dynamic Structure ◽  
Geomagnetic Indices ◽  
Solar Wind Parameters ◽  
Short Time ◽  
Physical Principles

Since the time scale of weak storms is about half the time scale of intense storms, it is troublesome and important to examine the solar wind parameters/interplanetary magnetic field (IMF) (E, v , P , T, N, and Bz) to evolve and affect to zonal geomagnetic indices (Kp, Dst, AE, and ap). In a severe storm, which usually has two main phases, solar parameters have enough time to react, but weak storms cannot find this time. They have to yield their reaction in a short time. One can find a weak storm in order to reveal and discuss the consistency of models that have proven themselves in severe and moderate storms in this study. I discuss weak storm (Dst = −46) on May 8, 2014, via solar wind parameters and zonal geomagnetic indices. The goal of the work is to realize the models applicable to the moderate and the strong storms for a weak storm. Hereby, all possible correlations between solar parameters and zonal indices are discussed in depth. I tried to obey the cause-effect relationship while creating mathematical models while not ignoring the physical principles. Therefore, the physical principles govern the study. The results are visualized with tables and graphs for the understanding of the dynamic structure of the storm.

Characteristic of Solar Wind Parameters and Geomagnetic Indices during Solar Flares

2018 ◽  
Vol 13 (S340) ◽  
pp. 257-258
Author(s):  
Roshan K. Mishra ◽  
Binod Adhikari ◽  
Drabindra Pandit ◽  
Narayan P. Chapagain
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Solar Flare ◽  
Solar Flares ◽  
High Speed ◽  
Solar Wind Velocity ◽  
Geomagnetic Indices ◽  
Solar Winds ◽  
Solar Wind Parameters

AbstractActive sun is characterized by compelling short-lived flash of solar eruption like solar flare, coronal mass ejections (CMEs), high-speed solar winds and solar energetic particles along with colossal release of energy and mass. This paper proposes a new method to evaluate solar wind parameters and geomagnetic indices based on wavelet analysis during the solar flares. The crucial role of IMF-Bz (interplanetary magnetic field) is examined for the two solar flares events. The key result obtained from our study is substantial dependence of solar flare intensity on IMF-Bz together with solar wind velocity. We also observed the duration of solar flares and their effect on ionospheric and ground based parameters.

scholarly journals Wavelet Analysis on Solar Wind Parameters and Geomagnetic Indices

Solar Physics ◽  
2012 ◽  
Vol 280 (2) ◽  
pp. 623-640 ◽  
Author(s):  
C. Katsavrias ◽  
P. Preka-Papadema ◽  
X. Moussas
Keyword(s):  
Solar Wind ◽  
Wavelet Analysis ◽  
Geomagnetic Indices ◽  
Solar Wind Parameters

Statistical analysis of solar wind parameters and geomagnetic indices during HILDCAA/HILDCAA ∗ occurrences between 1998 and 2007

2017 ◽  
Vol 60 (8) ◽  
pp. 1850-1865 ◽  
Author(s):  
Alan Prestes ◽  
Virginia Klausner ◽  
Arian Ojeda González ◽  
Silvio Leite Serra
Keyword(s):  
Solar Wind ◽  
Statistical Analysis ◽  
Geomagnetic Indices ◽  
Solar Wind Parameters

scholarly journals Comparison of the observed dependence of large-scale Birkeland currents on solar wind parameters with that obtained from global simulations

2011 ◽  
Vol 29 (10) ◽  
pp. 1809-1826 ◽  
Author(s):  
H. Korth ◽  
L. Rastätter ◽  
B. J. Anderson ◽  
A. J. Ridley
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Large Scale ◽  
Coupled Model ◽  
Total Current ◽  
Modeling Framework ◽  
Rate Of Increase ◽  
Solar Wind Parameters ◽  
The University ◽  
Birkeland Currents

Abstract. Spatial distributions of the large-scale Birkeland currents derived from magnetic field data acquired by the constellation of Iridium Communications satellites have been compared with global-magnetosphere magneto-hydrodynamic (MHD) simulations. The Iridium data, spanning the interval from February 1999 to December 2007, were first sorted into 45°-wide bins of the interplanetary magnetic field (IMF) clock angle, and the dependencies of the Birkeland currents on solar wind electric field magnitude, Eyz, ram pressure, psw, and Alfvén Mach number, MA, were then examined within each bin. The simulations have been conducted at the publicly-accessible Community Coordinated Modeling Center using the University of Michigan Space Weather modeling Framework, which features a global magnetosphere model coupled to the Rice Convection Model. In excess of 120 simulations with steady-state conditions were executed to yield the dependencies of the Birkeland currents on the solar wind and IMF parameters of the coupled model. Averaged over all IMF orientations, the simulation reproduces the Iridium statistical Birkeland current distributions with a two-dimensional correlation coefficient of about 0.8, and the total current agrees with the climatology averages to within 10%. The total current for individual events regularly exceeds those computed from statistical distributions by factors of ≥2, resulting in larger disparities between observations and simulations. The simulation results also qualitatively reflect the observed increases in total current with increasing Eyz and psw, but the model underestimates the rate of increase by up to 50%. The equatorward expansion and shift of the large-scale currents toward noon observed for increasing Eyz are also evident in the simulation current patterns. Consistent with the observations, the simulation does not show a significant dependence of the total current on MA.

scholarly journals Reconstruction of geomagnetic activity and near-Earth interplanetary conditions over the past 167 yr – Part 2: A new reconstruction of the interplanetary magnetic field

2013 ◽  
Vol 31 (11) ◽  
pp. 1979-1992 ◽  
Author(s):  
M. Lockwood ◽  
L. Barnard ◽  
H. Nevanlinna ◽  
M. J. Owens ◽  
R. G. Harrison ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Interplanetary Magnetic Field ◽  
Geomagnetic Activity ◽  
Flow Speed ◽  
Range Data ◽  
Solar Wind Flow ◽  
Annual Means ◽  
Solar Wind Parameters ◽  
The Imf

Abstract. We present a new reconstruction of the interplanetary magnetic field (IMF, B) for 1846–2012 with a full analysis of errors, based on the homogeneously constructed IDV(1d) composite of geomagnetic activity presented in Part 1 (Lockwood et al., 2013a). Analysis of the dependence of the commonly used geomagnetic indices on solar wind parameters is presented which helps explain why annual means of interdiurnal range data, such as the new composite, depend only on the IMF with only a very weak influence of the solar wind flow speed. The best results are obtained using a polynomial (rather than a linear) fit of the form B = χ · (IDV(1d) − β)α with best-fit coefficients χ = 3.469, β = 1.393 nT, and α = 0.420. The results are contrasted with the reconstruction of the IMF since 1835 by Svalgaard and Cliver (2010).

Fusion conditions in a finite-thickness gas-puff staged Z-pinch

1994 ◽  
Vol 52 (3) ◽  
pp. 365-371 ◽  
Author(s):  
Arshad M. Mirza ◽  
N. A. D. Khattak ◽  
M. Iqbal ◽  
G. Murtaza
Keyword(s):  
Magnetic Field ◽  
Time Scale ◽  
Rise Time ◽  
Axial Magnetic Field ◽  
Finite Thickness ◽  
Order Of Magnitude ◽  
Stabilization Effect ◽  
Pinch Current ◽  
Short Time ◽  
Z Pinch

We investigate the implosion of a dense τ-pinch plasma driven by an annular finite-thickness gas-puff Z-pinch. The imploding Z-pinch traps an axial magnetic field Bz, compressing it to large values in an extremely short time. The temporal variation of Bz then induces an azimuthal τ current on the surface of a fibre placed on the axis, with a rise time an order of magnitude shorter than the rise time of the Z-pinch current. Our numerical results demonstrate that, for a thick gas-puff layer, maximum compression occurs before the current peaks.We also find that at peak compression, fuel densities of the order of 1025 cm-3 and temperatures above 10 keV can be achieved on a time scale of the order of 0.1 ns. Thus a Lawson parameter nτ ≈ 1014 s cm-3 for a DT fibre becomes achievable. The snowplough effect in the Z-pinch exercises a stabilization effect on the growth of sausage and Rayleigh—Taylor instabilities. In the limit of a very thin gas-puff layer, previous results are fully recovered.

scholarly journals Azimuthally asymmetric ring current as a function of <i>D<sub>st</sub></i> and solar wind conditions

2004 ◽  
Vol 22 (8) ◽  
pp. 2989-2996 ◽  
Author(s):  
Y. P. Maltsev ◽  
A. A. Ostapenko
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Spatial Distribution ◽  
Interplanetary Magnetic Field ◽  
Ring Current ◽  
Dynamic Pressure ◽  
Solar Wind Dynamic Pressure ◽  
Magnetic Data ◽  
Under Five ◽  
Solar Wind Parameters

Abstract. Based on magnetic data, spatial distribution of the westward ring current flowing at |z|<3 RE has been found under five levels of Dst, five levels of the interplanetary magnetic field (IMF) z component, and five levels of the solar wind dynamic pressure Psw. The maximum of the current is located near midnight at distances 5 to 7 RE. The magnitude of the nightside and dayside parts of the westward current at distances from 4 to 9 RE can be approximated as Inight=1.75-0.041 Dst, Inoon=0.22-0.013 Dst, where the current is in MA. The relation of the nightside current to the solar wind parameters can be expressed as Inight=1.45-0.20 Bs IMF + 0.32 Psw, where BsIMF is the IMF southward component. The dayside ring current poorly correlates with the solar wind parameters.

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