The 04 – 10 September 2017 Sun–Earth Connection Events: Solar Flares, Coronal Mass Ejections/Magnetic Clouds, and Geomagnetic Storms

Solar Physics ◽  
2019 ◽  
Vol 294 (8) ◽  
Author(s):  
Chin-Chun Wu ◽  
Kan Liou ◽  
Ronald P. Lepping ◽  
Lynn Hutting
Keyword(s):  
Coronal Mass Ejections ◽  
Solar Flares ◽  
Geomagnetic Storms ◽  
Magnetic Clouds ◽  
Earth Connection

MAGNETIC CLOUDS: A SUBJECT OF SPACE WEATHER PREDICTION

2005 ◽  
Vol 20 (29) ◽  
pp. 6650-6653
Author(s):  
A. GERANIOS ◽  
M. VANDAS ◽  
E. ANTONIADOU ◽  
O. ZACHAROPOULOU
Keyword(s):  
Space Weather ◽  
Coronal Mass Ejections ◽  
Strong Influence ◽  
Geomagnetic Storms ◽  
Interplanetary Medium ◽  
Weather Prediction ◽  
Magnetic Clouds ◽  
The Sun ◽  
Time Intervals ◽  
The Earth

Magnetic clouds are ideal objects for solar-terrestrial studies because of their simplicity and their extended time intervals of southward and northward magnetic fields. Magnetic clouds constitute a significant subset of coronal mass ejections with remarkable characteristics in the interplanetary medium and a strong influence on the Earth's magnetosphere, giving rise to geomagnetic storms. The evolution of such a cloud from the neighborhood of the Sun up to the Earth is numerically simulated for two cases, without and with a presence of a faster moving shock front. Its influence on the magnetosphere can be seen by the triggered geomagnetic storm. Therefore, magnetic clouds are an important subject for space weather predictions.

Study of solar flares associated with Geoeffective CMEs

2018 ◽  
Vol 13 (S340) ◽  
pp. 163-164
Author(s):  
Veena Choithani ◽  
Rajmal Jain ◽  
Duggirala Pallamraju
Keyword(s):  
Solar Wind ◽  
Wind Speed ◽  
Solar Flare ◽  
Coronal Mass Ejections ◽  
Solar Flares ◽  
Geomagnetic Storms ◽  
Solar Wind Speed ◽  
Dst Index ◽  
In The Beginning ◽  
The Imf

AbstractWe study 30 solar flare events associated with coronal mass ejections (CMEs) that produced geomagnetic storms as measured in Dst index. Our study reveals that the magnitude of Dst index is significantly associated with maximum solar wind speed, peak of Bz component of the IMF and the product of peak Bz and solar wind speed (minimum and maximum). From our investigations, it can be inferred that CMEs travel with higher speed in the beginning and their speed reduces as they reach L1 location.

Prospective of coronal mass ejections, solar flares and geomagnetic storms

2014 ◽  
Vol 88 (11) ◽  
pp. 1127-1133 ◽  
Author(s):  
A. K. Singh ◽  
A. Tonk ◽  
R. Singh
Keyword(s):  
Coronal Mass Ejections ◽  
Solar Flares ◽  
Geomagnetic Storms

Solar flares, magnetic clouds, and geomagnetic storms

Solar Physics ◽  
1993 ◽  
Vol 143 (2) ◽  
pp. 365-372 ◽  
Author(s):  
K. G. Ivanov ◽  
A. F. Harshiladze ◽  
E. P. Romashets
Keyword(s):  
Solar Flares ◽  
Geomagnetic Storms ◽  
Magnetic Clouds

scholarly journals Radio Observation of Coronal Mass Ejections (CMEs) due to Flare Related Phenomenon on 7th March 2012

2014 ◽  
Vol 30 ◽  
pp. 243-256 ◽  
Author(s):  
Zety Sharizat Hamidi ◽  
C. Monstein ◽  
N.N.M. Shariff
Keyword(s):  
Solar Flare ◽  
Coronal Mass Ejections ◽  
Solar Flares ◽  
Current Knowledge ◽  
Radio Observation ◽  
Related Phenomenon ◽  
The Sun ◽  
Type Iii ◽  
Solar Burst ◽  
Earth Connection

On March 7th, 2012, an active region AR1429 has unleashed 2 major X-class solar flares. This flare is accompanied by a Coronal Mass Ejections (CMEs) event. A pair of unusually large solar flares early March 7, 2012 generated a Coronal Mass Ejection that was expected to reach Earth around midday March 8. In this case we focused on the second explosion of solar flare. It is found that the indication of signal potentially drives Coronal Mass Ejections (CMEs). There are a few types solar burst that can be observed, which is (i) an individual type III (ii) a complex type III (iii) subtype an H type II solar burst and (iv) type IV solar burst. The duration of solar burst is start from 1:02 UT to 2:00 UT. We also compare our results with the Geostationary Operational Environmental Satellites (GOES) data. Overall, one hour duration with a strong intensity burst are exploded strongly within the period. The fast drift type III burst has continued until 1:28 UT is associated with the large X 5.4 -class solar flares at 1:25:05 UT. It is undeniable that solar flare plays an important role in the Sun-Earth connection due to sudden changes of strong magnetic fields in the Sun’s corona. From our analysis, one possible reason behind the formation of this very complex, long duration of this loop is the magnetic reconnection and disruption of the loops which is observed during flare maximum. Until now, there has been an increasing interest in the space weather program has stimulated interest in this issue. A new experimental approach by e-CALLISTO with 24 hours monitoring and further development of a model of the theory are hoping to meet the current knowledge about the Sun behaviour.

scholarly journals Some kinematics of halo coronal mass ejections

2020 ◽  
Vol 29 (1) ◽  
pp. 81-88
Author(s):  
Virendra Kumar Verma ◽  
Nishant Mittal ◽  
Ramesh Chandra
Keyword(s):  
Coronal Mass Ejections ◽  
Solar Flares ◽  
Coronal Holes ◽  
Geomagnetic Disturbances ◽  
Class A ◽  
Heliospheric Physics ◽  
Class B ◽  
The Mean ◽  
Class C

AbstractWe present an investigation of halo coronal mass ejections (HCMEs) kinematics and other facts about the HCMEs. The study of HCMEs is very important because HCMEs are regarded as the main causes of heliospheric and geomagnetic disturbances. In this study, we have investigated 313 HCMEs observed during 1996-2012 by LASCO, coronal holes, and solar flares. We find that HCMEs are of two types: accelerated HCMEs and decelerated HCMEs. The mean space speed of HCMEs is 1283 km/s while the mean speed of decelerated HCMEs and accelerated HCMEs is 1349 km/s and 1174 km/s, respectively. The investigation shows that 1 (0.3%) HCME was associated with class A SXR, 14 (4.7%) HCMEs were associated with class B SXR-flares, 87 (29.4%) HCMEs were associated with class C SXR-flares, 125 (42.2%) HCMEs were associated with class M SXR-flares and 69 (23.3%) HCMEs were associated with class X SXR-flares. The speed of HCMEs increases with the importance of solar SXR-flares. The various results obtained in the present analysis are discussed in the light of the existing scenario of heliospheric physics.

Modeling of coronal mass ejections that caused particularly large geomagnetic storms using ENLIL heliosphere cone model

Space Weather ◽  
2011 ◽  
Vol 9 (6) ◽  
pp. n/a-n/a ◽  
Author(s):  
A. Taktakishvili ◽  
A. Pulkkinen ◽  
P. MacNeice ◽  
M. Kuznetsova ◽  
M. Hesse ◽  
...  
Keyword(s):  
Coronal Mass Ejections ◽  
Geomagnetic Storms ◽  
Cone Model

Investigating the Statistical Relationship between Coronal Mass Ejections and Solar Flares

2021 ◽  
Vol 85 (3) ◽  
pp. 234-237
Author(s):  
N. A. Barkhatov ◽  
V. G. Vorobjev ◽  
S. E. Revunov ◽  
E. A. Revunova
Keyword(s):  
Coronal Mass Ejections ◽  
Solar Flares ◽  
Statistical Relationship
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