scholarly journals Common solar wind drivers behind magnetic storm–magnetospheric substorm dependency

2018 ◽  
Vol 8 (1) ◽  
Author(s):  
Jakob Runge ◽  
Georgios Balasis ◽  
Ioannis A. Daglis ◽  
Constantinos Papadimitriou ◽  
Reik V. Donner
Keyword(s):  
Solar Wind ◽  
Magnetic Storm ◽  
Magnetospheric Substorm

scholarly journals Time scale of the largest imaginable magnetic storm

2013 ◽  
Vol 20 (1) ◽  
pp. 19-23 ◽  
Author(s):  
V. M. Vasyliūnas
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Magnetic Storm ◽  
Energy Content ◽  
Horizontal Magnetic Field ◽  
Order Of Magnitude ◽  
Magnetosphere Plasma ◽  
Time Required ◽  
Parameter Values ◽  
Magnetic Field Perturbation

Abstract. The depression of the horizontal magnetic field at Earth's equator for the largest imaginable magnetic storm has been estimated (Vasyliūnas, 2011a) as −Dst ~ 2500 nT, from the assumption that the total pressure in the magnetosphere (plasma plus magnetic field perturbation) is limited, in order of magnitude, by the minimum pressure of Earth's dipole field at the location of each flux tube. The obvious related question is how long it would take the solar wind to supply the energy content of this largest storm. The maximum rate of energy input from the solar wind to the magnetosphere can be evaluated on the basis either of magnetotail stress balance or of polar cap potential saturation, giving an estimate of the time required to build up the largest storm, which (for solar-wind and magnetospheric parameter values typical of observed superstorms) is roughly between ~2 and ~6 h.

Statistical Study of the Effect of Different Solar Wind Types on Magnetic Storm Generation During 1995–2016

2018 ◽  
Vol 58 (6) ◽  
pp. 737-743 ◽  
Author(s):  
L. A. Dremukhina ◽  
I. G. Lodkina ◽  
Y. I. Yermolaev
Keyword(s):  
Solar Wind ◽  
Magnetic Storm ◽  
Statistical Study

scholarly journals Extremely intense (SML ≤–2500 nT) substorms: isolated events that are externally triggered?

2015 ◽  
Vol 33 (5) ◽  
pp. 519-524 ◽  
Author(s):  
B. T. Tsurutani ◽  
R. Hajra ◽  
E. Echer ◽  
J. W. Gjerloev
Keyword(s):  
Solar Wind ◽  
Magnetic Fields ◽  
Magnetic Storm ◽  
Solar Wind Plasma ◽  
Magnetic Storms ◽  
Input Energy ◽  
Stored Energy ◽  
Ionospheric Currents ◽  
Interplanetary Magnetic Fields ◽  
Very High

Abstract. We examine particularly intense substorms (SML ≤–2500 nT), hereafter called "supersubstorms" or SSS events, to identify their nature and their magnetic storm dependences. It is found that these intense substorms are typically isolated events and are only loosely related to magnetic storms. SSS events can occur during super (Dst ≤–250 nT) and intense (−100 nT ≥ Dst >–250) magnetic storms. SSS events can also occur during nonstorm (Dst ≥–50 nT) intervals. SSSs are important because the strongest ionospheric currents will flow during these events, potentially causing power outages on Earth. Several SSS examples are shown. SSS events appear to be externally triggered by small regions of very high density (~30 to 50 cm−3) solar wind plasma parcels (PPs) impinging upon the magnetosphere. Precursor southward interplanetary magnetic fields are detected prior to the PPs hitting the magnetosphere. Our hypothesis is that these southward fields input energy into the magnetosphere/magnetotail and the PPs trigger the release of the stored energy.

Does magnetic storm generation depend on the solar wind type?

2017 ◽  
Vol 57 (5) ◽  
pp. 512-518 ◽  
Author(s):  
N. S. Nikolaeva ◽  
Yu. I. Yermolaev ◽  
I. G. Lodkina ◽  
M. Yu. Yermolaev
Keyword(s):  
Solar Wind ◽  
Magnetic Storm

Variations of geomagnetic thresholds of cosmic rays and magnetospheric parameters during different phases  of the storm of November 20, 2003

2021 ◽  
Author(s):  
Elena Vernova ◽  
Natalia Ptitsyna ◽  
Olga Danilova ◽  
Marta Tyasto
Keyword(s):  
Solar Wind ◽  
Cosmic Rays ◽  
Hysteresis Loop ◽  
Magnetic Storm ◽  
Cosmic Ray ◽  
Recovery Phase ◽  
Main Phase ◽  
Cutoff Rigidity ◽  
The Relationship ◽  
Current Systems

<div> <p>The correlations between variations in the geomagnetic cutoff rigidity of cosmic rays and the Dst and Kp geomagnetic indices and solar-wind and IMF parameters are calculated for the three phases of the magnetic storm of November 20–21, 2003: before the storm and during its main and recovery phases. The correlations are the strongest between variations in the cutoff rigidity and the Dst index during all stages. A significant correlation was recorded with the By component of IMF and the field magnitude B; the correlation with By dominated during the main phase, and the correlation with B was dominant during the recovery phase. There is also a high correlation with the dynamic parameters of solar activity during the main phase, especially with the solar-wind speed.</p> <div> <p>As far as we know, hysteresis phenomena have been discovered for the first time in the relationship between the cosmic-ray cutoff rigidities and the parameters of the helio- and magnetosphere on the scale of the magnetic storm (with Moscow station as an example). Loop-like patterns formed, because the trajectories of variations in the cutoff rigidities versus the studied parameters during storm intensification (development of current systems) did not coincide with the trajectories during the recovery phase (decay of current systems). The correlations of the cutoff rigidities with Dst and Kp indices were characterized by a narrow hysteresis loop, and their correlations with the IMF parameters were characterized by a wide hysteresis loop. The hysteresis loops for the relationship between the cutoff rigidities and solar-wind density and pressure were disordered.</p> </div> </div>

scholarly journals April 2000 magnetic storm: Solar wind driver and magnetospheric response

2002 ◽  
Vol 107 (A12) ◽  
pp. SMP 15-1-SMP 15-21 ◽  
Author(s):  
K. Emilia J. Huttunen ◽  
Hannu E. J. Koskinen ◽  
Tuija I. Pulkkinen ◽  
Antti Pulkkinen ◽  
Minna Palmroth ◽  
...  
Keyword(s):  
Solar Wind ◽  
Magnetic Storm
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