Statistical Characteristics on SEPs, Radio-Loud CMEs, Low Frequency Type II and Type III Radio Bursts Associated with Impulsive and Gradual ... View Full Text


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Article Info

DATE

2020-07-11

AUTHORS

P. Pappa Kalaivani, A. Shanmugaraju, O. Prakash, R.-S. Kim

ABSTRACT

We have statistically analyzed a set of 115 low frequency (Deca-Hectometer wavelengths range) type II and type III bursts associated with major Solar Energetic Particle (SEP: Ep > 10 MeV) events and their solar causes such as solar flares and coronal mass ejections (CMEs) observed from 1997 to 2014. We classified them into two sets of events based on the duration of the associated solar flares:75 impulsive flares (duration < 60 min) and 40 gradual flares (duration > 60 min).On an average, the peak flux (integrated flux) of impulsive flares × 2.9 (0.32 J m−2) is stronger than that of gradual flares M6.8 (0.24 J m−2). We found that impulsive flare-associated CMEs are highly decelerated with larger initial acceleration and they achieved their peak speed at lower heights (− 27.66 m s−2 and 14.23 Ro) than the gradual flare-associated CMEs (6.26 m s−2 and 15.30 Ro), even though both sets of events have similar sky-plane speed (space speed) within LASCO field of view. The impulsive flare-associated SEP events (Rt = 989.23 min: 2.86 days) are short lived and they quickly reach their peak intensity (shorter rise time) when compared with gradual flares associated events (Rt = 1275.45 min: 3.34 days). We found a good correlation between the logarithmic peak intensity of all SEPs and properties of CMEs (space speed: cc = 0.52, SEcc = 0.083), and solar flares (log integrated flux: cc = 0.44, SEcc = 0.083). This particular result gives no clear cut distinction between flare-related and CME-related SEP events for this set of major SEP events. We derived the peak intensity, integrated intensity, duration and slope of these bursts from the radio dynamic spectra observed by Wind/WAVES. Most of the properties (peak intensity, integrated intensity and starting frequency) of DH type II bursts associated with impulsive and gradual flare events are found to be similar in magnitudes. Interestingly, we found that impulsive flare-associated DH type III bursts are longer, stronger and faster (31.30 min, 6.43 sfu and 22.49 MHz h−1) than the gradual flare- associated DH type III bursts (25.08 min, 5.85 sfu and 17.84 MHz h−1). In addition, we also found a significant correlation between the properties of SEPs and key parameters of DH type III bursts. This result shows a closer association of peak intensity of the SEPs with the properties of DH type III radio bursts than with the properties DH type II radio bursts, atleast for this set of 115 major SEP events. More... »

PAGES

61-85

References to SciGraph publications

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  • 2017-02-23. Characteristics of events with metric-to-decahectometric type II radio bursts associated with CMEs and flares in relation to SEP events in ASTROPHYSICS AND SPACE SCIENCE
  • 2015-01-07. Relationship between Solar Energetic Particles and Properties of Flares and CMEs: Statistical Analysis of Solar Cycle 23 Events in SOLAR PHYSICS
  • 2009-01-16. The SOHO/LASCO CME Catalog in EARTH, MOON, AND PLANETS
  • 2012-01-17. A Twin-CME Scenario for Ground Level Enhancement Events in SPACE SCIENCE REVIEWS
  • 2016-05. Relationships Between Interplanetary Coronal Mass Ejection Characteristics and Geoeffectiveness in the Rising Phase of Solar Cycles 23 and 24 in SOLAR PHYSICS
  • 2012-09-27. Kinematics and Flare Properties of Radio-Loud CMEs in SOLAR PHYSICS
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    http://scigraph.springernature.com/pub.10.1007/s11038-020-09533-9

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    25 schema:description We have statistically analyzed a set of 115 low frequency (Deca-Hectometer wavelengths range) type II and type III bursts associated with major Solar Energetic Particle (SEP: Ep > 10 MeV) events and their solar causes such as solar flares and coronal mass ejections (CMEs) observed from 1997 to 2014. We classified them into two sets of events based on the duration of the associated solar flares:75 impulsive flares (duration < 60 min) and 40 gradual flares (duration > 60 min).On an average, the peak flux (integrated flux) of impulsive flares × 2.9 (0.32 J m−2) is stronger than that of gradual flares M6.8 (0.24 J m−2). We found that impulsive flare-associated CMEs are highly decelerated with larger initial acceleration and they achieved their peak speed at lower heights (− 27.66 m s−2 and 14.23 Ro) than the gradual flare-associated CMEs (6.26 m s−2 and 15.30 Ro), even though both sets of events have similar sky-plane speed (space speed) within LASCO field of view. The impulsive flare-associated SEP events (Rt = 989.23 min: 2.86 days) are short lived and they quickly reach their peak intensity (shorter rise time) when compared with gradual flares associated events (Rt = 1275.45 min: 3.34 days). We found a good correlation between the logarithmic peak intensity of all SEPs and properties of CMEs (space speed: cc = 0.52, SEcc = 0.083), and solar flares (log integrated flux: cc = 0.44, SEcc = 0.083). This particular result gives no clear cut distinction between flare-related and CME-related SEP events for this set of major SEP events. We derived the peak intensity, integrated intensity, duration and slope of these bursts from the radio dynamic spectra observed by Wind/WAVES. Most of the properties (peak intensity, integrated intensity and starting frequency) of DH type II bursts associated with impulsive and gradual flare events are found to be similar in magnitudes. Interestingly, we found that impulsive flare-associated DH type III bursts are longer, stronger and faster (31.30 min, 6.43 sfu and 22.49 MHz h−1) than the gradual flare- associated DH type III bursts (25.08 min, 5.85 sfu and 17.84 MHz h−1). In addition, we also found a significant correlation between the properties of SEPs and key parameters of DH type III bursts. This result shows a closer association of peak intensity of the SEPs with the properties of DH type III radio bursts than with the properties DH type II radio bursts, atleast for this set of 115 major SEP events.
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    33 LASCO field
    34 M6.8
    35 SEP events
    36 SEPs
    37 Wind/WAVES
    38 acceleration
    39 addition
    40 association
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    43 bursts
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    45 characteristics
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    47 close association
    48 coronal mass ejections
    49 correlation
    50 cut distinction
    51 distinction
    52 duration
    53 dynamic spectra
    54 ejection
    55 energetic particle events
    56 events
    57 field
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    60 flux
    61 good correlation
    62 gradual flares
    63 height
    64 impulsive flares
    65 initial acceleration
    66 intensity
    67 key parameters
    68 large initial acceleration
    69 low height
    70 magnitude
    71 major SEP events
    72 major solar energetic particle events
    73 mass ejections
    74 parameters
    75 particle events
    76 particular results
    77 peak flux
    78 peak intensity
    79 peak speed
    80 properties
    81 properties of CMEs
    82 properties of SEP
    83 radio bursts
    84 radio dynamic spectra
    85 radio-loud (RL) Coronal Mass Ejections
    86 results
    87 set
    88 set of events
    89 significant correlation
    90 slope
    91 solar causes
    92 solar energetic particle events
    93 solar flares
    94 spectra
    95 speed
    96 statistical characteristics
    97 type II
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    99 type II radio bursts
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    104 schema:name Statistical Characteristics on SEPs, Radio-Loud CMEs, Low Frequency Type II and Type III Radio Bursts Associated with Impulsive and Gradual Flares
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