Catalogue of 55–80 MeV solar proton events extending through solar cycles 23 and 24

Paassilta, Miikka; Raukunen, Osku; Vainio, R.; Валтонен, Э.; Papaioannou, Athanasios; Siipola, Robert; Riihonen, E.; Dierckxsens, M.; Crosby, Norma; Malandraki, O.; Heber, B.; Klein, Karl‐Ludwig

doi:10.1051/swsc/2017013

Cited by 41 publications

(33 citation statements)

References 34 publications

(50 reference statements)

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“…While CXD‐equipped GPS satellites have been on orbit since 2001, the first of 11 Block IIF satellites was launched in May 2010 and the last seven satellites of Block IIF were launched across 2014 and 2015. Large SEP events have occurred rarely in Solar Cycle 24 (Paassilta et al, ), and so we have selected these SEP events as they have high peak fluxes (thus spanning a large range of measured flux) as determined by the NOAA Space Weather Prediction Center, are well studied, and were measured by a sufficient number of the CXD instruments.…”

Section: Data Descriptionmentioning

confidence: 99%

Cross Calibration of the GPS Constellation CXD Proton Data With GOES EPS

et al. 2018

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Accurate proton flux measurements of the near‐Earth environment are essential to the understanding of many phenomena which have a direct impact on our lives. Currently, there is only a small set of satellites capable of performing these measurements which makes certain studies and analyses difficult. This paper details the capabilities of the Combined X‐ray Dosimeter (CXD), flown on 21 satellites of the Global Positioning System constellation, as it relates to proton measurements. We present a cross calibration of the CXD with the Energetic Particle Sensor (EPS) onboard the Geostationary Operational Environmental Satellite operated by the National Oceanic and Atmospheric Administration. By utilizing Solar Energetic Particle Events when both sets of satellites were operational we have orders of magnitude in flux and energy to compare against. Robust statistical analyses show that the CXD and Geostationary Operational Environmental Satellite flux calculations are similar and that for proton energies >30 MeV the CXD fluxes are on average within 20% of EPS. Although the CXD has a response to protons as low as 6 MeV, the sensitivity at energies below 20 MeV is reduced and so flux comparisons of these are generally worse. Integral flux values >10 MeV are typically within 40% of EPS. These calibrated CXD data sets will give researchers capabilities to study solar proton access to the inner magnetosphere down to L ~ 4 near the equatorial plane at high temporal cadence.

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Section: Data Descriptionmentioning

confidence: 99%

Cross Calibration of the GPS Constellation CXD Proton Data With GOES EPS

et al. 2018

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“…This catalog was updated on-line 4 to cover the period 1997−2015. A recent summary over the period 1996−2016 is presented by Paassilta et al (2017).…”

Section: Introductionmentioning

confidence: 99%

The Wind/EPACT Proton Event Catalog (1996 – 2016)

2018

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We present the finalized catalog of solar energetic proton events detected by Wind/EPACT instrument over the period 1996−2016. Onset times, peak times, peak proton intensity and onset-to-peak proton fluence are evaluated for the two available energy channels, at about 25 and 50 MeV. We describe the procedure utilized to identify the proton events and to relate them to their solar origin (in terms of flares and coronal mass ejections). The statistical relationships between the energetic protons and their origin (linear and partial correlation analysis) are reported and discussed in view of earlier findings. Finally, the different trends found in the first eight years of solar cycles 23 and 24 are discussed. Miteva et al. 1 https://ngdc.noaa.gov/stp/satellite/goes/datanotes.html 2 http://umbra.nascom.nasa.gov/SEP/ 3 1 pfu = 1 proton/(cm 2 s sr) 4 http://server.sepserver.eu/, status: July 2017 5 The SEPEM 7.23−10.45 reference proton event list: http://dev.sepem.oma.be/help/event ref. html SOLA: Mitevaetal.tex; 3 January 2018; 1:39; p. 2 Wind/EPACT proton catalog the database with a focus on either energy-dependent statistics (Dierckxsens et al., 2015), or, among others, the distribution with respect to NOAA Solar Radiation Storm scale (Papaioannou et al., 2016). Recently, a new list of high energy protons (1995−2015), >500 MeV from the Electron Proton Helium Instrument [EPHIN] instrument aboard SOHO (Müller-Mellin et al., 1995) was presented by Kühl et al. (2017).Among the proton catalogs covering only SC23 is the 25 MeV proton database from the IMP-8 instrument (Cane, Richardson, and von Rosenvinge, 2010), as well as other listings 6 as noted by Papaioannou et al. (2016). Other particle lists using GOES and SOHO/COSTEP (Müller-Mellin et al., 1995) data were created for the purpose of testing forecasting procedures (Laurenza et al., 2009;Posner, 2007).Numerous statistical studies between SEP events and their solar origin (flares and CMEs) are known. Different works use differential or integral proton fluxes, flare class or/and fluence, CME projected speed or/and angular width, investigate the longitudinal effects, probability of occurrence or propose new statistical methods. The strength of the correlation between the protons and their solar origin is used to argue in favor of or against the particle driver. Below we outline studies covering at least one solar cycle. Presenting a complete account on all previous works is not the objective of this study.A comprehensive study is the energy dependent statistics provided by Dierckxsens et al. (2015) based on re-calibrated data from GOES and IMP-8 instruments over 10 energy channels (from 5 to 200 MeV) and in the entire SC23 (using SEPEM data 7 , Crosby et al., 2015). The work provides results based on differential and integral proton intensities. The main result is the larger correlation between flares and high energy protons, whereas the low energy protons correlate better with CME speed. Among the other works over SC23 that provide also new particle lists are: Cane, R...

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“…The catalog of Paassilta et al (2017) was used to select the proton events for this study. The catalog consists of proton events observed by the Energetic and Relativistic Nuclei and Electron experiment (ERNE) (Torsti et al, 1995) on board the Solar and Heliospheric Observatory (SOHO) spacecraft at energies 55 -80 MeV during the years 1996 -2016.…”

Section: E Valtonenmentioning

confidence: 99%

“…It seems plausible that protons in Category 2 events were accelerated by CME-driven shocks high in the solar corona. Large delays of protons with respect to type III onsets in the events where protons were released after the electrons suggest late acceleration or release of protons close to the Sun, but the exact mechanism causing the delay remained unclear.The catalog of Paassilta et al (2017) was used to select the proton events for this study. The catalog consists of proton events observed by the Energetic and Relativistic Nuclei and Electron experiment (ERNE) (Torsti et al, 1995) on board the Solar and Heliospheric Observatory (SOHO) spacecraft at energies 55 -80 MeV during the years 1996 -2016.…”

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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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Catalogue of 55–80 MeV solar proton events extending through solar cycles 23 and 24

Cited by 41 publications

References 34 publications

Cross Calibration of the GPS Constellation CXD Proton Data With GOES EPS

Cross Calibration of the GPS Constellation CXD Proton Data With GOES EPS

The Wind/EPACT Proton Event Catalog (1996 – 2016)

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

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