Solar radio bursts: Implications to the origin of in situ particles

Miteva, Rositsa

doi:10.31401/sungeo.2018.02.04

Cited by 2 publications

(2 citation statements)

References 20 publications

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“…Fixes SEP intensity levels (e.g., large SEP events) also introduces a bias when performing correlation coefficients, namely towards reduced correlation with flare class and enhanced correlation with CME speed. This could be one of the explanation of the reported differences in correlation coefficients by earlier works (see comparison done in [38]). Other reasons include different identifications for the solar origin (flares/CMEs) of the same proton event, energy dependence effect (see trends found by [10]), different flare/CME databases used.…”

Section: Summary and Discussionmentioning

confidence: 68%

Solar energetic particle catalogs: Assumptions, uncertainties and validity of reports

Miteva¹,

Samwel²,

Costa-Duarte³

2018

Journal of Atmospheric and Solar-Terrestrial Physics

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The aim of this work is to summarize the main underlying assumptions, simplifications and uncertainties while studying solar energetic particles (SEPs).In general, numerous definitions are used for the evaluation of a given SEP parameter and these different methods lead to different outcomes for a given particle event. Several catalogs of SEP events from various instruments are currently available; however, each catalog is specific to the adopted data and analysis. We investigate the differences while comparing several SEP catalogs and outline probable reasons. We focus on SEP statistical studies and quantify the influences of the particle intensity magnitude, solar origin location and projection effects. We found that different definitions and criteria used for these parameters change the values of the correlation coefficients between the SEPs and their solar origin. AbstractThis template helps you to create a properly formatted L A T E X manuscript.

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Section: Summary and Discussionmentioning

confidence: 68%

Solar energetic particle catalogs: Assumptions, uncertainties and validity of reports

Miteva¹,

Samwel²,

Costa-Duarte³

2018

Journal of Atmospheric and Solar-Terrestrial Physics

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“…Traditionally solar energetic particle events have been divided into two classes of impulsive and gradual events (Cane, McGuire, and von Rosenvinge, 1986). Cane, Richardson, and von Rosenvinge (2010) and more recently Kim et al (2014Kim et al ( , 2015, Gopalswamy et al (2015Gopalswamy et al ( , 2016bGopalswamy et al ( , 2017, Miteva (2018) have presented divisions of SEP events in types or groups deviating from this traditional classification. Our Category 1 events are "impulsive" in the sense that they have high intensity rise rates, short rise times, the protons are released low in the corona, the events originate from magnetically well-connected regions, and are associated with short-duration X-ray flares.…”

Section: Time-of-maximum Energy Spectramentioning

confidence: 99%

Properties of High-Energy Solar Particle Events Associated with Solar Radio Emissions

2019

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We have analysed 58 high-energy proton events and 36 temporally related nearrelativistic electron events from the years 1997 -2015 for which the velocity dispersion analysis of the first-arriving particles gave the apparent path lengths between 1 and 3 AU. We investigated the dependence of the characteristics of the proton events on the associations of type II, III, and IV radio bursts. We also examined the properties of the soft X-ray flares and coronal mass ejections associated with these events. All proton events were associated with decametric type III radio bursts, while type IV emission was observed only in the meter wavelengths in some of the events (32/58). Almost all proton events (56/58) were associated with radio type II bursts: 11 with metric (m) type II only, 11 with decametrichectometric (DH) only, and 34 with type II radio bursts at both wavelength ranges. By examining several characteristics of the proton events, we discovered that the proton events can be divided into two categories. The characteristics of events belonging to the same category were similar, while they significantly differed between events in different categories. The distinctive factors between the categories were the wavelength range of the associated type II radio emission and the temporal relation of the proton release with respect to the type II onset. In Category 1 are the events which were associated with only metric type II emission or both m and DH type II and the release time of protons was before the DH type II onset (18/56 events). Category 2 consists of the events which were associated with only DH type II emission or both m and DH type II and the protons were released at or after the DH type II onset (31/56 events). For seven of the 56 events we were not able to determine a definite category due to timing uncertainties. The events in Category 1 had significantly higher intensity rise rates, shorter rise times, lower release heights, and harder energy spectra than B D. Ameri dahame@utu.fi E. ValtonenCategory 2 events. Category 1 events also originated from magnetically well-connected regions and had only small time differences between the proton release times and the type III onsets. The soft X-ray flares for these events had significantly shorter rise times and durations than for Category 2 events. We found 36 electron events temporally related to the proton events, which fulfilled the same path length criterion as the proton events. We compared the release times of protons and electrons at the Sun, and discovered that in 19 of the 36 events protons were released almost simultaneously (within ± 7 minutes) with the electrons, in 16 events protons were released later than the electrons, and in one event electrons were released after the protons. The simultaneous proton and electron events and the delayed proton events did not unambiguously fall in the two categories of proton events, although most of the events in which the protons were released after the electrons belonged to Category 2. We conclude that acceleration ...

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Solar radio bursts: Implications to the origin of in situ particles

Cited by 2 publications

References 20 publications

Solar energetic particle catalogs: Assumptions, uncertainties and validity of reports

Solar energetic particle catalogs: Assumptions, uncertainties and validity of reports

Properties of High-Energy Solar Particle Events Associated with Solar Radio Emissions

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