scholarly journals Radial variation of solar wind electrons inside a magnetic cloud observed at 1 and 5 AU

2000 ◽  
Vol 105 (A12) ◽  
pp. 27269-27275 ◽  
Author(s):  
R. M. Skoug ◽  
W. C. Feldman ◽  
J. T. Gosling ◽  
D. J. McComas ◽  
D. B. Reisenfeld ◽  
...  
Keyword(s):  
Solar Wind ◽  
Magnetic Cloud ◽  
Radial Variation

ESTABLISHING THE ORIENTATION OF SHOCK WAVE PLANE OF SOLAR WIND MAGNETIC CLOUD FOR CONCLUSIONS ABOUT THE LEVEL OF AURORAL SUBSTORM ACTIVITY

2019 ◽  
Vol 17 (1) ◽  
pp. 195-202 ◽  
Author(s):  
N. A. Barkhatov ◽  
S. E. Revunov ◽  
M. V. Mukhina ◽  
M. L. Gruzdeva ◽  
O. T. Cherney ◽  
...  
Keyword(s):  
Shock Wave ◽  
Solar Wind ◽  
Magnetic Cloud ◽  
Auroral Substorm ◽  
Substorm Activity

scholarly journals Reflected solar wind ions and downward accelerated ionospheric ions during the January 1997 magnetic cloud event

1998 ◽  
Vol 25 (15) ◽  
pp. 2979-2982 ◽  
Author(s):  
D. L. Dempsey ◽  
J. L. Burch ◽  
M. M. Huddleston ◽  
C. J. Pollock ◽  
J. H. Waite ◽  
...  
Keyword(s):  
Solar Wind ◽  
Magnetic Cloud

scholarly journals Magnetic cloud field intensities and solar wind velocities

1998 ◽  
Vol 25 (7) ◽  
pp. 963-966 ◽  
Author(s):  
W. D. Gonzalez ◽  
A. L. Clúa de Gonzalez ◽  
A. Dal Lago ◽  
B. T. Tsurutani ◽  
J. K. Arballo ◽  
...  
Keyword(s):  
Solar Wind ◽  
Magnetic Cloud ◽  
Wind Velocities

The solar wind magnetic cloud of October 18–20, 1995: effect on ionosphere of the Russian Asian region

2001 ◽  
Vol 27 (8) ◽  
pp. 1381-1384 ◽  
Author(s):  
V.I. Kurkin ◽  
N.M. Polekh ◽  
O.M. Pirog ◽  
L.V. Chistyakova ◽  
G.A. Zherebtsov
Keyword(s):  
Solar Wind ◽  
Magnetic Cloud ◽  
Asian Region

scholarly journals On the Geoeffectiveness Structure of Solar Wind-Magnetosphere Coupling Functions during Intense Storms

2011 ◽  
Vol 2011 ◽  
pp. 1-13 ◽  
Author(s):  
B. Olufemi Adebesin ◽  
S. Oluwole Ikubanni ◽  
J. Stephen Kayode
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Magnetic Cloud ◽  
Recovery Phase ◽  
Flow Speed ◽  
Event Correlation ◽  
Phase Duration ◽  
Event Identification ◽  
Solar Wind Flow ◽  
The Magnetic Field

The geoeffectiveness of some coupling functions for the Solar Wind-Magnetosphere Interaction had been studied. 58 storms with peak Dst < −100 nT were used. The result showed that the interplanetary magnetic field Bz appeared to be more relevant with the magnetic field B (which agreed with previous results). However, both the V (solar wind flow speed) and Bz factors in the interplanetary dawn-dusk electric field (V×Bz) are effective in the generation of very intense storms (peak Dst < −250 nT) while “intense” storms (−250 nT ≤ peak Dst < −100 nT) are mostly enhanced by the Bz factor alone (in most cases). The southward Bz duration BT seems to be more relevant for Dst < −250 nT class of storms and invariably determines the recovery phase duration. Most of the storms were observed to occur at midnight hours (i.e., 2100–0400 UT), having a 41.2% incidence rate, with high frequency between 2300 UT and 0000 UT. 62% of the events were generated as a result of Magnetic Cloud (MC), while 38% were generated by complex ejecta. The B-Bz relation for the magnetic cloud attained a correlation coefficient of 0.8922, while it is 0.7608 for the latter. Conclusively, Bz appears to be the most geoeffective factor, and geoeffectiveness should be a factor that depends on methods of event identification and classification as well as the direction of event correlation.

scholarly journals Modeling the Lunar Wake Response to a CME Using a Hybrid PIC Model

2022 ◽  
Vol 3 (1) ◽  
pp. 4
Author(s):  
Anthony P. Rasca ◽  
Shahab Fatemi ◽  
William M. Farrell
Keyword(s):  
Solar Wind ◽  
Magnetic Cloud ◽  
Plasma Sheath ◽  
Wake Region ◽  
Plasma Parameters ◽  
Particle In Cell ◽  
Lunar Wake ◽  
Wind Spacecraft ◽  
Upstream Solar Wind ◽  
Mass Ejection

Abstract In the solar wind, a low-density wake region forms downstream of the nightside lunar surface. In this study, we use a series of 3D hybrid particle-in-cell simulations to model the response of the lunar wake to a passing coronal mass ejection (CME). Average plasma parameters are derived from the Wind spacecraft located at 1 au during three distinct phases of a passing halo (Earth-directed) CME on 2015 June 22. Each set of plasma parameters, representing the shock/plasma sheath, a magnetic cloud, and plasma conditions we call the mid-CME phase, are used as the time-static upstream boundary conditions for three separate simulations. These simulation results are then compared with results that use nominal solar wind conditions. Results show a shortened plasma void compared to nominal conditions and a distinctive rarefaction cone originating from the terminator during the CME’s plasma sheath phase, while a highly elongated plasma void reforms during the magnetic cloud and mid-CME phases. Developments of electric and magnetic field intensification are also observed during the plasma sheath phase along the central wake, while electrostatic turbulence dominates along the plasma void boundaries and 2–3 lunar radii R M downstream in the central wake during the magnetic cloud and mid-CME phases. The simulations demonstrate that the lunar wake responds in a dynamic way with the changes in the upstream solar wind during a CME.

SUPERSUBSTORM ON 28 MAY 2011 – GEOMAGNETIC EFFECTS IN THE GLOBAL SCALE

2021 ◽  
Vol 44 ◽  
pp. 12-15
Author(s):  
I.V. Despirak ◽  
◽  
N.G. Kleimenova ◽  
A.A. Lubchich ◽  
P.V. Setsko ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Ring Current ◽  
Magnetic Measurements ◽  
Magnetic Cloud ◽  
Dynamic Pressure ◽  
Global Scale ◽  
Strong Magnetic Storm ◽  
Evening Sector ◽  
Typical Scenario

For this analysis, we selected the supersubstorm (SSS) occurred during the strong magnetic storm on 28 May 2011 (SYM/H~100 nT). The ground-based magnetic effects of SSS have been studied basing on the data from the global SuperMAG, INTERMAGNET and IMAGE magnetometer networks, as well as on the magnetic measurements by the ionospheric satellite AMPERE system. According to the SML- index behavior, the SSS event maximum was identified at ~09:00 UT on 28 May 2011 (SML= ~-2600 nT). The SSS occurred during the passage of the magnetic cloud in the solar wind. Before the SSS, the BZ component of the Interplanetary Magnetic Field (IMF) was negative, the IMF BY component was positive, and the local jump in the solar wind dynamic pressure was registered. We found that the SSS developed in the magnetosphere in the global scale. A strong westward electrojet was observed at auroral latitudes from the evening side to the dayside. In contrast to the typical scenario of a classical substorm, a very intense eastward electrojet was detected in the afternoon-evening sector. That may be a result of the formation of an additional partial ring current during the supersubstorm.

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