Correlation Analyses Between the Characteristic Times of Gradual Solar Energetic Particle Events and the Properties of Associated Coronal Mass Ejections

Pan, Zihan; Wang, C. B.; Wang, Yuming; Xue, Xianghui

doi:10.1007/s11207-011-9763-0

Cited by 9 publications

(8 citation statements)

References 40 publications

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“…As with any coronagraph observations, significant plane of the sky projection effects occur in the speed (and also width) if the CME does not originate near the limb of the Sun relative to the observing spacecraft. Cone models have been developed to help correct for projection (e.g., Howard et al, 1982;Zhao, Plunkett and Liu, 2002;Xie, Ofman and Lawrence, 2004;Xue, Wang and Dou, 2005;Michalek, Gopalswamy and Yashiro, 2007;Na et al, 2013;Nicewicz and Michalek, 2014, and references therein) but have not been widely used in SEP studies (see however, Pan et al, 2011).…”

Section: Cme Catalogsmentioning

confidence: 99%

The Properties of Solar Energetic Particle Event-Associated Coronal Mass Ejections Reported in Different CME Catalogs

Richardson

Rosenvinge

Cane³

2015

Sol Phys

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We compare estimates of the speed and width of coronal mass ejections (CMEs) in several catalogs for the CMEs associated with ∼ 200 solar energetic particle (SEP) events in 2006-2013 that included 25 MeV protons. The catalogs used are: CDAW, CACTUS, SEEDS and CORIMP, all derived from observations by the LASCO coronagraphs on the SOHO spacecraft, the CACTUS catalog derived from the COR2 coronagraphs on the STEREO-A and -B spacecraft, and the DONKI catalog, which uses observations from SOHO and the STEREO spacecraft. We illustrate how, for this set of events, CME parameters can differ considerably in each catalog. The well-known correlation between CME speed and proton event intensity is shown to be similar for most catalogs, but this is largely because it is determined by a few large particle events associated with fast CMEs, and small events associated with slow CMEs. Intermediate particle events "shuffle" in position when speeds from different catalogs are used. Quadrature spacecraft CME speeds do not improve the correlation. CME widths also vary widely between catalogs, and are influenced by plane of the sky projection and how the width is inferred from the coronagraph images. The high degree of association (∼ 50%) between the 25 MeV proton events and "full halo" (360 owidth) CMEs as defined in the CDAW catalog is removed when other catalogs are considered. Using CME parameters from the quadrature spacecraft, the SEP intensity is correlated with CME width, which is also correlated with CME speed.

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Section: Cme Catalogsmentioning

confidence: 99%

The Properties of Solar Energetic Particle Event-Associated Coronal Mass Ejections Reported in Different CME Catalogs

Richardson

Rosenvinge

Cane³

2015

Sol Phys

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“…4). Secondary peaks correspond to impulsive SEP events, with rise times 3 h, and gradual ones, with rise times~33 h. An extremely gradual event exhibited a rise time of up to~55 h. As expected by theoretical (e.g., Mikić & Lee, 2006) and observational (e.g., Pan et al, 2011) works, rise times statistically decrease for increasingly westward heliographic source locations. Figure 22 a also highlights this; d all SEP events in our sample invariably correspond to major solar eruptions, associated with at least M-class flares and fast CMEs with average speed 1810 ± 750 km/s ( Table 3).…”

Section: Summary Conclusion and Outlookmentioning

confidence: 53%

Analysis and interpretation of inner-heliospheric SEP events with the ESA Standard Radiation Environment Monitor (SREM) onboard the INTEGRAL and Rosetta Missions

Georgoulis

Papaioannou

Sandberg

et al. 2018

J. Space Weather Space Clim.

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Using two heliospheric vantage points, we study 22 solar energetic particle (SEP) events, 14 of which were detected at both locations. SEP proton events were detected during the declining phase of solar cycle 23 (November 2003-December 2006 by means of two nearly identical Standard Radiation Environment Monitor (SREM) units in energies ranging between 12.6 MeV and 166.3 MeV. In this work we combine SREM data with diverse solar and interplanetary measurements, aiming to backtrace solar eruptions from their impact in geospace (i.e., from L1 Lagrangian point to Earth's magnetosphere) to their parent eruptions at the Sun's low atmosphere. Our SREM SEP data support and complement a consistent inner-heliospheric description of solar eruptions (solar flares and coronal mass ejections [CMEs]) and their magnetospheric impact. In addition, they provide useful information on the understanding of the origin, acceleration, and propagation of SEP events at multi-spacecraft settings. All SEP events in our sample originate from major eruptions consisting of major (>M-class) solar flares and fast (>1800 km/s, on average), overwhelmingly (>78%) halo, CMEs. All but one SEP event studied are unambiguously associated with shock-fronted CMEs, suggesting a CME-driven shock acceleration mechanism. Moreover, a significant correlation is found between the SEP event peak and the onset of the storm sudden commencement, that might help improve prediction of magnetospheric disturbances. In general, SEP events correlate better with interplanetary (i.e., in-situ; L1-based) than with solar eruption features. Our findings support (a) the routine use of cost-effective SREM units, or future improvements thereof, for the detection of SEP events and (b) their implementation in multi-spacecraft settings as a means to improve both the physical understanding of SEP events and their forecasting.

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“…Particles that arrive later, even well before the peak, may undergo scattering, possibly by irregularities in the magnetic field, turbulence, etc., in the corona and interplanetary space. Past studies either showed no correlation (Kahler 2005;Pan et al 2011) or a weak inverse correlation (Kahler 2013) between TO and v CM E . We followed Kahler (2013) in analyzing the grouping of v CM E into four subgroups and calculating median values-here we showed averages instead of medians.…”

Section: Discussionmentioning

confidence: 92%

“…In this paper, we presented the statistical trends found in a large number of events observed at GOES, STEREO-A and STEREO-B. Moreover, we analyzed mostly solar cycle 24 events, whereas similar statistical studies dealt with solar cycle 23 events (e.g., Kahler 2005Kahler , 2013Pan et al 2011) or partially included solar cycle 24 events (e.g., Papaioannou et al 2016). Another difference from previous studies of SEP timescales is that we used the CME source longitude relative to the footpoint of the Parker spiral (∆Φ) rather than to the observer.…”

Section: Discussionmentioning

confidence: 99%

Statistical Analysis of the Relation between Coronal Mass Ejections and Solar Energetic Particles

Kihara,

Huang,

Nishimura

et al. 2020

Preprint

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To improve the forecasting capability of impactful solar energetic particle (SEP) events, the relation between coronal mass ejections (CMEs) and SEP events needs to be better understood. Here we present a statistical study of SEP occurrences and timescales with respect to the CME source locations and speeds, considering all 257 fast (v CM E ≥ 900 km s −1 ) and wide (angular width ≥ 60 • ) CMEs that occurred between December 2006 and October 2017. We associate them with SEP events at energies above 10 MeV. Examination of the source region of each CME reveals that CMEs more often accompany a SEP event if they originate from the longitude of E20 -W100 relative to the observer. However, a SEP event could still be absent if the CME is < 2000 km s −1 . For the associated CME-SEP pairs, we compute three timescales for each of the SEP events, following Kahler (2005Kahler ( , 2013; namely the timescale of the onset (TO), the rise time (TR), and the duration (TD). They are correlated with the longitude of the CME source region relative to the footpoint of the Parker spiral (∆Φ) and v CM E . The TO tends to be short for |∆Φ| <60 • . This trend is weaker for TR and TD. The SEP timescales are only weakly correlated with v CM E . Positive correlations of both TR and TD with v CM E are seen in poorly connected (large |∆Φ|) events. Additionally, TO appears to be negatively correlated with v CM E for events with small |∆Φ|.

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Correlation Analyses Between the Characteristic Times of Gradual Solar Energetic Particle Events and the Properties of Associated Coronal Mass Ejections

Cited by 9 publications

References 40 publications

The Properties of Solar Energetic Particle Event-Associated Coronal Mass Ejections Reported in Different CME Catalogs

The Properties of Solar Energetic Particle Event-Associated Coronal Mass Ejections Reported in Different CME Catalogs

Analysis and interpretation of inner-heliospheric SEP events with the ESA Standard Radiation Environment Monitor (SREM) onboard the INTEGRAL and Rosetta Missions

Statistical Analysis of the Relation between Coronal Mass Ejections and Solar Energetic Particles

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