scholarly journals Flare related geomagnetic storms with coronal mass ejections, radio bursts and jumps in solar wind plasma density

2021 ◽  
Vol 10 (2) ◽  
Author(s):  
Shiva Soni ◽  
Preetam Singh Gour
Keyword(s):  
Solar Wind ◽  
Plasma Density ◽  
Coronal Mass Ejections ◽  
Geomagnetic Storms ◽  
Solar Wind Plasma ◽  
Radio Bursts

H-Cmes and Ii-Type Radio Bursts Related Intense Geomagnetic Storms in Relation With Interplanetary Magnetic Field and Solar Wind Disturbances

2012 ◽  
Vol 2 (10) ◽  
pp. 1-3 ◽  
Author(s):  
Praveen Kumar Gupta ◽  
◽  
Puspraj Singh Puspraj Singh ◽  
Puspraj Singh Puspraj Singh ◽  
P. K. Chamadia P. K. Chamadia
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Interplanetary Magnetic Field ◽  
Geomagnetic Storms ◽  
Radio Bursts ◽  
Solar Wind Disturbances

scholarly journals Super Strong Geomagnetic Storms and their Relation with Energetic Solar Features and Disturbances in Solar wind Plasma Parameters

2011 ◽  
Vol 2 (1) ◽  
pp. 152-156
Author(s):  
P.L.Verma P.L.Verma ◽  
◽  
Manoj Kumar Mishra ◽  
Monika Mishra ◽  
Preetum Singh ◽  
...  
Keyword(s):  
Solar Wind ◽  
Geomagnetic Storms ◽  
Solar Wind Plasma ◽  
Plasma Parameters

High-latitude ionospheric response to co-rotating interaction region- and coronal mass ejection-driven geomagnetic storms revealed by GPS tomography and ionosondes

2010 ◽  
Vol 466 (2123) ◽  
pp. 3391-3408 ◽  
Author(s):  
D. Pokhotelov ◽  
P. T. Jayachandran ◽  
C. N. Mitchell ◽  
M. H. Denton
Keyword(s):  
Solar Wind ◽  
Coronal Mass Ejection ◽  
Plasma Density ◽  
Large Scale ◽  
Geomagnetic Storms ◽  
Interaction Region ◽  
Electron Content ◽  
Polar Cap ◽  
Total Electron ◽  
Mass Ejection

Positive ionospheric anomalies induced in the polar cap region by co-rotating interaction region (CIR)- and coronal mass ejection (CME)-driven geomagnetic storms are analysed using four-dimensional tomographic reconstructions of the ionospheric plasma density based on measurements of the total electron content along ray paths of GPS signals. The results of GPS tomography are compared with ground-based observations of F region plasma density by digital ionosondes located in the Canadian Arctic. It is demonstrated that CIR- and CME-driven storms can produce large-scale polar cap anomalies of similar morphology in the form of the tongue of ionization (TOI) that appears on the poleward edge of the mid-latitude dayside storm-enhanced densities in positive ionospheric storms. The CIR-driven event of 14–16 October 2002 was able to produce ionospheric anomalies (TOI) comparable to those produced by the CME-driven storms of greater Dst magnitude. From the comparison of tomographic reconstructions and ionosonde data with solar wind measurements, it appears that the formation of large-scale polar cap anomalies is controlled by the orientation of the interplanetary magnetic field (IMF) with the TOI forming during the periods of extended southward IMF under conditions of high solar wind velocity.

scholarly journals The Interplanetary and Magnetospheric Causes of Geomagnetically Induced Currents (GICs) > 10 A in the Mäntsälä Finland Pipeline: 1999 through 2019

2021 ◽  
Author(s):  
Bruce Tsurutani ◽  
Rajkumar Hajra
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Coronal Mass Ejections ◽  
Solar Wind Plasma ◽  
Local Times ◽  
Induced Current ◽  
Geomagnetically Induced Currents ◽  
Geomagnetically Induced Current ◽  
The Third ◽  
Induced Currents

The interplanetary and magnetospheric causes of intense geomagnetically induced current (GIC) > 10 A and > 30 A events during 21 years (1999 through 2019) at the Mäntsälä, Finland (57.9° magnetic latitude) gas pipeline have been studied. Although forward shocks and substorms are predominant causes of intense GICs, some newly discovered geoeffective interplanetary features are: solar wind plasma parcel (PP) impingements, possible interplanetary magnetic field (IMF) northward (Bn) and southward (Bs) turnings, and reverse shocks. The PPs are possibly the loop and filament portions of coronal mass ejections (CMEs).   From a study of > 30 A GIC events, it is found that supersubstorm (SSS: SML < -2500 nT) and intense substorm (-2500 nT < SML < -2000 nT) auroral electrojet intensifications are the most frequent (76%) cause of all of these GIC events. These events occur most often (76%) in superstorm (SYM-H ≤ -250 nT) main phases, but they can occur in other storm phases and lesser intensity storms as well. After substorms, PPs were the most frequent causes of Mäntsälä GIC > 30 A events. Forward shocks were the third most frequent cause of the > 30 A events. Shock-related GICs were observed to occur at all local times.   The two “Halloween” superstorms of 29-30 and 30-31 October 2003 produced by far the greatest number of GICs in the interval of study (9 > 30 A GICs and 168 > 10 A GICs). In the first Halloween superstorm, a shock-triggered SSS (SML < -3548 nT) caused 33, 57, 51 and 52 A GICs. The 57 A GIC was the most intense event of the superstorm and of this study. Equally intense magnetic storms were also studied but their related GICs were far less numerous and less intense.

scholarly journals Relationship between geomagnetic storm development and the solar wind parameter ß

2021 ◽  
Vol 7 (4) ◽  
pp. 24-32
Author(s):  
Nadezhda Kurazhkovskaya ◽  
Oleg Zotov ◽  
Boris Klain
Keyword(s):  
Solar Wind ◽  
Geomagnetic Storms ◽  
Activity Cycle ◽  
Solar Activity Cycle ◽  
Solar Wind Plasma ◽  
Recovery Phase ◽  
Plasma Pressure ◽  
Superposition Method ◽  
Solar Wind Parameter ◽  
Dst Index

We have analyzed the dynamics of solar wind and interplanetary magnetic field (IMF) parameters during the development of 933 isolated geomagnetic storms, observed over the period from 1964 to 2010. The analysis was carried out using the epoch superposition method at intervals of 48 hrs before and 168 hrs after the moment of Dst minimum. The geomagnetic storms were selected by the type of storm commencement (sudden or gradual) and by intensity (weak, moderate, and strong). The dynamics of the solar wind and IMF parameters was compared with that of the Dst index, which is an indicator of the development of geomagnetic storms. The largest number of storms in the solar activity cycle is shown to occur in the years of minimum average values (close in magnitude to 1) of the solar wind parameter β (β is the ratio of plasma pressure to magnetic pressure). We have revealed that the dynamics of the Dst index is similar to that of the β parameter. The duration of the storm recovery phase follows the characteristic recovery time of the β parameter. We have found out that during the storm main phase the β parameter is close to 1, which reflects the maximum turbulence of solar wind plasma fluctuations. In the recovery phase, β returns to background values β~2‒3.5. We assume that the solar wind plasma turbulence, characterized by the β parameter, can play a significant role in the development of geomagnetic storms.

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