Global expansion of the dayside magnetopause for long-duration radial IMF events: Statistical study on GOES observations

2016 ◽  
Vol 121 (7) ◽  
pp. 6480-6492 ◽  
Author(s):  
Jong-Sun Park ◽  
Jih-Hong Shue ◽  
Khan-Hyuk Kim ◽  
Gilbert Pi ◽  
Zdeněk Němeček ◽  
...  
Keyword(s):  
Statistical Study ◽  
Global Expansion ◽  
Long Duration ◽  
Dayside Magnetopause

A statistical study of accelerated flow events at the dayside magnetopause

1994 ◽  
Vol 99 (A8) ◽  
pp. 14815 ◽  
Author(s):  
L. Scurry ◽  
C. T. Russell ◽  
J. T. Gosling
Keyword(s):  
Statistical Study ◽  
Dayside Magnetopause ◽  
Accelerated Flow

scholarly journals A statistical study of plasmaspheric plumes and ionospheric outflows observed at the dayside magnetopause

2016 ◽  
Vol 121 (1) ◽  
pp. 492-506 ◽  
Author(s):  
S. H. Lee ◽  
H. Zhang ◽  
Q.‐G. Zong ◽  
A. Otto ◽  
H. Rème ◽  
...  
Keyword(s):  
Statistical Study ◽  
Dayside Magnetopause

scholarly journals A Statistical Study of Slow-Mode Shocks Observed by MMS in the Dayside Magnetopause

2018 ◽  
Vol 45 (10) ◽  
pp. 4675-4684
Author(s):  
N. K. Walia ◽  
K. Seki ◽  
M. Hoshino ◽  
T. Amano ◽  
N. Kitamura ◽  
...  
Keyword(s):  
Statistical Study ◽  
Slow Mode ◽  
Dayside Magnetopause

scholarly journals Statistical study of transient plasma structures in magnetotail lobes and plasma sheet boundary layer: Interball-1 observations

2002 ◽  
Vol 20 (3) ◽  
pp. 329-340 ◽  
Author(s):  
E. E. Grigorenko ◽  
A. Fedorov ◽  
L. M. Zelenyi
Keyword(s):  
Plasma Sheet ◽  
Statistical Study ◽  
Spatial Distributions ◽  
Neutral Sheet ◽  
Plasma Sheet Boundary Layer ◽  
Time Intervals ◽  
Interplanetary Magnetic Fields ◽  
Long Duration ◽  
Generation Mechanisms ◽  
Transient Plasma

Abstract. The present paper is devoted to the statistical study of plasma structures observed at the interface between magnetospheric lobes and the plasma sheet at distances of 15–25 RE . The majority of the registered structures are bursty earthward ion streams with energies about 10–30 keV known as "beamlets". The paper describes the results of beamlet statistical analysis for different interplanetary magnetic fields (IMF), clock-angles and various magnetospheric conditions. It is shown that the energy of beamlets increases monotonously with a distance from the neutral sheet (NS) during slightly southward IMF and quiet magnetospheric conditions. Under these conditions, beamlets are observed up to 5–6 RE over the NS. In contrast, the beamlet energy decreases with increasing distance from the NS if the IMF is northward, and the region of beamlet observation becomes much wider up to 12 RE above the NS. The same (inverse) beamlet energy dependence on the distance from the NS is also registered during active magnetospheric periods. Yet, the plasma structures of various duration with quasi-isotropic ion velocity distributions resembling the plasma of the plasma sheet (PS) were observed in the same region. Statistical study performed for various IMF clock-angles demonstrates the clear difference in the spatial distributions of such plasma structures for two extreme IMF directions. When IMF is primarily northward, PS-like plasma fills the lobe region almost entirely and could be associated with the PS expansions. For primarily southward IMF time intervals, the probability of observing PS-like structures of long duration sharply decreases with the increasing distance from the NS, but PS-like structures of short durations (< 500 s) are distributed almost uniformly up to 12 RE above the NS. This feature cannot be described in terms of the PS flapping motions and requires another explanation. Relevance and limitations of the existing models attempting to explain the generation mechanisms of these transient structures are briefly discussed in the concluding part of the paper.Key words. Magnetospheric physics (magnetotail; magnetotail boundary layers; plasma sheet)

scholarly journals A Statistical Study to Determine the Origin of Long-duration Gamma-Ray Flares

2018 ◽  
Vol 864 (1) ◽  
pp. 39 ◽  
Author(s):  
L. M. Winter ◽  
V. Bernstein ◽  
N. Omodei ◽  
M. Pesce-Rollins
Keyword(s):  
Statistical Study ◽  
Gamma Ray ◽  
Long Duration

The LDE-Type Flare Occurrence (1969-1993)

1994 ◽  
Vol 144 ◽  
pp. 279-282
Author(s):  
A. Antalová
Keyword(s):  
Time Series ◽  
Fourier Analysis ◽  
Sunspot Cycle ◽  
List Type ◽  
Type Number ◽  
Solar Cycles ◽  
Type Iv ◽  
Long Duration ◽  
Cycle Maximum ◽  
Flare Index

AbstractThe occurrence of LDE-type flares in the last three cycles has been investigated. The Fourier analysis spectrum was calculated for the time series of the LDE-type flare occurrence during the 20-th, the 21-st and the rising part of the 22-nd cycle. LDE-type flares (Long Duration Events in SXR) are associated with the interplanetary protons (SEP and STIP as well), energized coronal archs and radio type IV emission. Generally, in all the cycles considered, LDE-type flares mainly originated during a 6-year interval of the respective cycle (2 years before and 4 years after the sunspot cycle maximum). The following significant periodicities were found:• in the 20-th cycle: 1.4, 2.1, 2.9, 4.0, 10.7 and 54.2 of month,• in the 21-st cycle: 1.2, 1.6, 2.8, 4.9, 7.8 and 44.5 of month,• in the 22-nd cycle, till March 1992: 1.4, 1.8, 2.4, 7.2, 8.7, 11.8 and 29.1 of month,• in all interval (1969-1992):a)the longer periodicities: 232.1, 121.1 (the dominant at 10.1 of year), 80.7, 61.9 and 25.6 of month,b)the shorter periodicities: 4.7, 5.0, 6.8, 7.9, 9.1, 15.8 and 20.4 of month.Fourier analysis of the LDE-type flare index (FI) yields significant peaks at 2.3 - 2.9 months and 4.2 - 4.9 months. These short periodicities correspond remarkably in the all three last solar cycles. The larger periodicities are different in respective cycles.

Statistical Study of the Rotation Effect of Am Stars

1976 ◽  
Vol 32 ◽  
pp. 675-683
Author(s):  
Keiichi Kodaira
Keyword(s):  
Statistical Study ◽  
Rotation Velocity ◽  
General View ◽  
Slow Rotation ◽  
Rotation Effect

SummaryExcess of [m1] index of Am stars, relative to normal stars, is statistically found to be correlated with rotation velocity; the coefficient is estimated at ∆׀m1׀ /∆V(km/sec) ˜ - 0.0007 among Am stars. This result supports the general view that slow rotation is essential for Am phenomena.

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