Statistical Analysis of Impulsiveness and Rise Phase Duration of Solar Flares in the He II 304 Angstrom Chromospheric Line

2021 ◽  
Author(s):  
Cole Tamburri ◽  
Maria Kazachenko ◽  
Adam Kowalski
Keyword(s):  
Statistical Analysis ◽  
Solar Flares ◽  
Phase Duration ◽  
Chromospheric Line ◽  
Rise Phase

scholarly journals Statistical research into low-power solar flares. Main phase duration

2017 ◽  
pp. 5-16 ◽  
Author(s):  
Александр Боровик ◽  
Aleksandr Borovik ◽  
Антон Жданов ◽  
Anton Zhdanov
Keyword(s):  
Statistical Analysis ◽  
Low Power ◽  
Solar Flares ◽  
Main Phase ◽  
Electronic Database ◽  
Statistical Research ◽  
Phase Duration ◽  
Long Duration ◽  
Time Parameters ◽  
Using Data

This paper is a sequel to earlier papers on time parameters of solar flares in the Hα line. Using data from the International Flare Patrol, an electronic database of solar flares for the period 1972–2010 has been created. The statistical analysis of the duration of the main phase has shown that it increases with increas-ing flare class and brightness. It has been found that the duration of the main phase depends on the type and features of development of solar flares. Flares with one brilliant point have the shortest main phase; flares with several intensity maxima and two-ribbon flares, the longest one. We have identified more than 3000 cases with an ultra-long duration of the main phase (more than 60 minutes). For 90 % of such flares the duration of the main phase is 2–3 hrs, but sometimes it reaches 12 hrs.

scholarly journals Statistical research into low-power solar flares. Main phase duration

2017 ◽  
Vol 3 (4) ◽  
pp. 5-16 ◽  
Author(s):  
Александр Боровик ◽  
Aleksandr Borovik ◽  
Антон Жданов ◽  
Anton Zhdanov
Keyword(s):  
Statistical Analysis ◽  
Low Power ◽  
Solar Flares ◽  
Main Phase ◽  
Electronic Database ◽  
Statistical Research ◽  
Phase Duration ◽  
Long Duration ◽  
Time Parameters ◽  
Using Data

This paper is a sequel to earlier papers on time parameters of solar flares in the Hα line. Using data from the International Flare Patrol, an electronic database of solar flares for the period 1972–2010 has been created. The statistical analysis of the duration of the main phase has shown that it increases with increasing flare class and brightness. It has been found that the duration of the main phase depends on the type and features of development of solar flares. Flares with one brilliant point have the shortest main phase; flares with several intensity maxima and two-ribbon flares, the longest one. We have identified more than 3000 cases with an ultra-long duration of the main phase (more than 60 minutes). For 90 % of such flares the duration of the main phase is 2–3 hrs, but sometimes it reaches 12 hrs.

Statistical analysis of soft X-ray solar flares during solar cycles 22, 23, and 24

2021 ◽  
Vol 366 (1) ◽  
Author(s):  
Bo Xiong ◽  
Ting Wang ◽  
Xiaolin Li ◽  
Yunxing Yin
Keyword(s):  
Statistical Analysis ◽  
Solar Flares ◽  
Solar Cycles ◽  
X Ray

On a possible explanation of chromospheric line asymmetries of solar flares

Solar Physics ◽  
1996 ◽  
Vol 166 (2) ◽  
pp. 437-440 ◽  
Author(s):  
M. D. Ding ◽  
C. Fang
Keyword(s):  
Solar Flares ◽  
Chromospheric Line

scholarly journals Electrons and X-Ray Emission of Solar Flares

1990 ◽  
Vol 142 ◽  
pp. 409-413
Author(s):  
V. G. Kurt
Keyword(s):  
Solar Activity ◽  
Statistical Analysis ◽  
Solar Flare ◽  
Frequency Dependence ◽  
Power Law ◽  
Solar Flares ◽  
X Rays ◽  
Fast Electrons ◽  
X Ray ◽  
Flare Frequency

A statistical analysis of solar flare X-rays and interplanetary particle fluxes, measured onboard VENERA-13, 14 Spacecraft, was performed. The correlation of fluences for different manifestations of solar flares is strong, especially for fast electrons and hard and soft X-ray emissions. Frequency dependence on fluence value ϵi for practically all Kinds of solar flare emission can be described by power law ν (ϵ > ϵO) ∼ ϵ−0.45±0.15 which does not change significantly with solar activity. For different Hα flare importances the values of ϵi were obtained. It is proposed that appearance of certain energy flare frequency is strongly dependent on some scale factor.

Solar Energetic Particle Events at the Rise Phase of the 23rd Solar Activity Cycle Registered aboard the Spacecraft “INTERBALL-2”

2000 ◽  
Vol 179 ◽  
pp. 251-254
Author(s):  
Vladislav Timofeev ◽  
Sergey Starodubtsev
Keyword(s):  
Solar Activity ◽  
Solar Flares ◽  
Energetic Particle ◽  
Solar Energetic Particle ◽  
Activity Cycle ◽  
Solar Activity Cycle ◽  
Solar Energetic Particle Events ◽  
Mass Ejection ◽  
Rise Phase ◽  
23Rd Solar Activity Cycle

AbstractThe experiment with 10K-80 aboard the INTER-BALL-2 (which detects protons with energies > 7, 27–41, 41–58, 58–88, 88–180 and 180–300 MeV) registered six events of the solar energetic particle (SEP) increase. These events are during the initial rise phase of the 23rd solar activity cycle. Solar flares with the SEP generation are accompanied by coronal mass ejection (CME). Here we analyze the dynamics of the differential energy spectrum at different phases of the SEP increase.

A statistical analysis of solar flares in 1996 – 2002

2004 ◽  
Vol 28 (2) ◽  
pp. 166-173
Author(s):  
Gui-ming Le ◽  
Yan-hong Chen
Keyword(s):  
Statistical Analysis ◽  
Solar Flares

Statistical analysis of ionospheric responses to solar flares in the solar cycle 23

2013 ◽  
Vol 118 (1) ◽  
pp. 576-582 ◽  
Author(s):  
Huijun Le ◽  
Libo Liu ◽  
Yiding Chen ◽  
Weixing Wan
Keyword(s):  
Statistical Analysis ◽  
Solar Cycle ◽  
Solar Flares ◽  
Solar Cycle 23

scholarly journals A statistical analysis of the soft X-ray profiles of solar flares

1989 ◽  
Vol 104 (2) ◽  
pp. 161-164
Author(s):  
G. Pearce ◽  
R.A. Harrison
Keyword(s):  
Statistical Analysis ◽  
Solar Flare ◽  
Solar Flares ◽  
Intensity Profile ◽  
Imaging Spectrometer ◽  
X Ray ◽  
X Ray Imaging ◽  
Selection Of

We undertake a statistical analysis of the soft X-ray (3.5 – 5.5 keV) profiles of solar flares as observed with the Hard X-ray Imaging Spectrometer on the SMM. The durations, maximum intensities and intensity profiles of the flares are examined. The properties of the “typical” solar flare are discussed. The distributions of the measured parameters with respect to one another reveal some interesting results. In common with past studies, we conclude that there is no evidence to suggest that more than one type of event is being viewed, despite a desire evident in the literature to place events into distinct groups. We also conclude that commonly held views about the relatonships between flare duration and intensity, profile asymmetries and intensity etc.. are in error. For more details of the flare events, the selection of data and the method of analysis, the reader is referred to Pearce and Harrison (1988).

Statistical Analysis of Reconnection Inflows in Solar Flares Observed withSOHOEIT

2006 ◽  
Vol 637 (2) ◽  
pp. 1122-1134 ◽  
Author(s):  
Noriyuki Narukage ◽  
Kazunari Shibata
Keyword(s):  
Statistical Analysis ◽  
Solar Flares
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