A study of solar energetic particle events of 1997–2006: Their composition and associations

Cane, H. V.; Richardson, I. G.; Rosenvinge, T. T. von

doi:10.1029/2009ja014848

Cited by 175 publications

(241 citation statements)

References 33 publications

(51 reference statements)

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“…The event selection is based on two previously published works, the comprehensive SEP catalog given by Cane, Richardson, and von Rosenvinge (2010) and a few events that were added from Klein et al (2011). We selected SEP events associated with flares with peak soft X-ray (SXR) flux 9×10 −6 W s −2 (GOES class C9) which were located on the solar disk including limb events (i.e.…”

Section: Discussionmentioning

confidence: 99%

“…The association rate is slightly lower for the western ICME/vicinity SEP events (83 %) than for the eastern ones. The reliability of the association rates calculated here depends on the correct SEP-parent activity identification adopted from Cane, Richardson, and von Rosenvinge (2010). During the detailed analysis of the eastern events however, we found that for three No-association cases the parent flare/CME might be a later event pair that is associated with an EIT disturbance.…”

Section: Sep Events and Eit Waves During Solar Cycle 23: Overall Assomentioning

confidence: 99%

“…Solar energetic particle events with origin at western [W] helio-longitudes and associated EIT disturbances, flares and CMEs. We list the SEP event date, the proton onset at 1 AU from Cane, Richardson, and von Rosenvinge (2010), the EIT wave association and time of first front observation, the SXR flare importance, start time, and longitude and finally the linear speed and angular width [AW] of the associated CME. a: identified in the SOHO/EIT 304Å channel; Hα: flare longitude from the Hα reports in the Solar Geophysical Data; I/S/V: SEP events propagating in ICME/Solar wind/Vicinity of an ICME; K: events from Klein et al (2011) For a positively identified EIT wave we also give the time when the disturbance was first observed.…”

Section: Flares and Cmesmentioning

confidence: 99%

“…The properties of the SEPassociated CMEs, e.g. CME linear (projected) speed and first appearance in the C2 coronagraph of the Large Angle and Spectrometric Coronagraph Experiment (LASCO-C2) field of view are taken from the SOHO/LASCO CME catalog at cdaw.gsfc.nasa.gov/CME list/, whereas the angular width [AW] is adopted from Cane, Richardson, and von Rosenvinge (2010). Table 1.…”

Section: Flares and Cmesmentioning

confidence: 99%

“…We adopted the proposed solar origin for each SEP event from Cane, Richardson, and von Rosenvinge (2010), but cross-checked the flare and CME characteristics. We used the Solar Geophysical Data reports at ftp.ngdc.noaa.gov/STP/SOLAR DATA/SGD PDFversion/, the online GOES flare list (under IDL-SolarSoft), and/or the information provided at www.SolarMonitor.org.…”

Section: Flares and Cmesmentioning

confidence: 99%

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Solar Energetic Particles and Associated EIT Disturbances in Solar Cycle 23

et al. 2014

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We explore the link between solar energetic particles (SEPs) observed at 1 AU and large-scale disturbances propagating in the solar corona, named after the Extreme ultraviolet Imaging Telescope (EIT) as EIT waves, which trace the lateral expansion of a coronal mass ejection (CME). A comprehensive search for SOHO/EIT waves was carried out for 179 SEP events during Solar Cycle 23 (1997 -2006). 87 % of the SEP events were found to be accompanied by EIT waves. In order to test if the EIT waves play a role in the SEP acceleration, we compared their extrapolated arrival time at the footpoint of the Parker spiral with the particle onset in the 26 eastern SEP events that had no direct magnetic connection to the Earth. We find that the onset of proton events was generally consistent with this scenario. However, in a number of cases the first near-relativistic electrons were detected too early. Furthermore, the electrons had in general only weakly anisotropic pitch-angle distributions. This poses a problem for the idea that the SEPs were accelerated by the EIT wave or in any other spatially confined region in the low corona. The presence of weak electron anisotropies in SEP events from the eastern hemisphere suggests that transport processes in interplanetary space, including cross-field diffusion, play a role in giving the SEPs access to a broad range of helio-longitudes.

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Section: Discussionmentioning

confidence: 99%

Section: Sep Events and Eit Waves During Solar Cycle 23: Overall Assomentioning

confidence: 99%

Section: Flares and Cmesmentioning

confidence: 99%

Section: Flares and Cmesmentioning

confidence: 99%

Section: Flares and Cmesmentioning

confidence: 99%

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Solar Energetic Particles and Associated EIT Disturbances in Solar Cycle 23

et al. 2014

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Influence of interplanetary coronal mass ejections on the peak intensity of solar energetic particle events

Lario

Karelitz

2014

JGR Space Physics

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We study whether the presence of coronal mass ejections (CMEs) in interplanetary space (ICMEs) affects the maximum intensity of solar energetic particle (SEP) events. We compute the maximum intensity of 175-315 keV electron and 9-15, 15-40, and 40-80 MeV proton fluxes measured during the prompt component of 147 western SEP events observed near Earth throughout solar cycle 23. When using in situ observations to determine the presence and location of preceding ICMEs during SEP events, we find that, over the ensemble of events, those observed either within a preceding ICME or when a preceding ICME is beyond the observer's location have, on average, larger peak intensities than the events observed in absence of ICMEs. The few events observed when an Earth-directed ICME is located between the Sun and the observer tend to have lower 9-15 and 15-40 MeV proton peak intensities than the events without preceding ICMEs; the differences are not significant for 175-315 keV electron peak intensities. When using coronagraph observations to determine the presence of preceding CMEs, we find that, over the ensemble of events, those events (Case P) occurring within 24 h after the launch of a CME from the same active region as the primary CME generating the SEP event tend to have higher peak intensities than those events (Case NP) occurring without a preceding CME. The differences between the average peak intensities of these two event cases (P and NP) are smaller when we exclude events observed when a prior ICME is already located at or beyond Earth.

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What flare and CME parameters control the occurrence of solar proton events?

Park

Moon

2014

JGR Space Physics

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In this study we examine the occurrence probabilities of solar proton events (SPEs) and their peak fluxes depending on both flare and coronal mass ejection (CME) parameters: flare peak flux, longitude, impulsive time, CME linear speed, and angular width. For this we use the NOAA SPEs, their associated X-ray flares, and CME from 1997 to 2011. We divide the data into 16 subgroups according to the flare and CME parameters and estimate the SPE probabilities for the subgroups. The three highest probabilities are found for the following subgroups: (1) fast full halo (55.3%) and fast partial halo (42.9%) CMEs associated with strong flares from the western region and (2) slow full halo CMEs associated with strong flares from the western region (31.6%). It is noted that the events whose SPE probabilities are nearly 0% belong to the following subgroups: (1) slow and fast partial halo CMEs from the eastern region, (2) slow partial halo CMEs from the western region, and (3) slow full halo CMEs from the eastern region. These results show that important parameters to control SPE occurrences are CME linear speed, angular width, and source longitude, which can be understood by the piston-driven shock formation of fast CMEs and magnetic field connectivity from the source site to the Earth. It is also shown that when the subgroups are separately considered by flare impulsive time and source longitude, the correlation coefficients between the observed and the predicted SPE peak fluxes are greatly improved.

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A study of solar energetic particle events of 1997–2006: Their composition and associations

Cited by 175 publications

References 33 publications

Solar Energetic Particles and Associated EIT Disturbances in Solar Cycle 23

Solar Energetic Particles and Associated EIT Disturbances in Solar Cycle 23

Influence of interplanetary coronal mass ejections on the peak intensity of solar energetic particle events

What flare and CME parameters control the occurrence of solar proton events?

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