The SOHO/LASCO CME Catalog

Gopalswamy, N.; Yashiro, S.; Michałek, G.; Stenborg, G.; Vourlidas, A.; Freeland, S.; Howard, R. A.

doi:10.1007/s11038-008-9282-7

Cited by 554 publications

(469 citation statements)

References 30 publications

Supporting

Mentioning

443

Contrasting

Unclassified

Order By: Relevance

“…However, only C2 and C3 data are being used since C1 was disabled in June 1998. The CME data utilized in this study are primarily derived by the LASCO CME Catalog 2 at http://cdaw.gsfc.nasa.gov/ CME_list/ (Gopalswamy et al 2009). The basic CME characteristics employed in our study are: -t CME : first appearance of the CME in the C2 field of view, -v CME : mean velocity determined from the linear fit to the height-time measurements, 1 R s = 695 700 km.…”

Section: Cme Datasetmentioning

confidence: 99%

Solar flares, coronal mass ejections and solar energetic particle event characteristics

Papaioannou

Sandberg

Anastasiadis

et al. 2016

J. Space Weather Space Clim.

142

129

View full text Add to dashboard Cite

A new catalogue of 314 solar energetic particle (SEP) events extending over a large time span from 1984 to 2013 has been compiled. The properties as well as the associations of these SEP events with their parent solar sources have been thoroughly examined. The properties of the events include the proton peak integral flux and the fluence for energies above 10, 30, 60 and 100 MeV. The associated solar events were parametrized by solar flare (SF) and coronal mass ejection (CME) characteristics, as well as related radio emissions. In particular, for SFs: the soft X-ray (SXR) peak flux, the SXR fluence, the heliographic location, the rise time and the duration were exploited; for CMEs the plane-of-sky velocity as well as the angular width were utilized. For radio emissions, type III, II and IV radio bursts were identified. Furthermore, we utilized element abundances of Fe and O. We found evidence that most of the SEP events in our catalogue do not conform to a simple two-class paradigm, with the 73% of them exhibiting both type III and type II radio bursts, and that a continuum of event properties is present. Although, the so-called hybrid or mixed events are found to be present in our catalogue, it was not possible to attribute each SEP event to a mixed/hybrid sub-category. Moreover, it appears that the start of the type III burst most often precedes the maximum of the SF and thus falls within the impulsive phase of the associated SF. At the same time, type III bursts take place within %5.22 min, on average, in advance from the time of maximum of the derivative of the SXR flux (Neupert effect). We further performed a statistical analysis and a mapping of the logarithm of the proton peak flux at E > 10 MeV, on different pairs of the parent solar source characteristics. This revealed correlations in 3-D space and demonstrated that the gradual SEP events that stem from the central part of the visible solar disk constitute a significant radiation risk. The velocity of the associated CMEs, as well as the SXR peak flux and fluence, are all fairly significantly correlated to both the proton peak flux and the fluence of the SEP events in our catalogue. The strongest correlation to SEP characteristics is manifested by the CME velocity.

show abstract

Section: Cme Datasetmentioning

confidence: 99%

Solar flares, coronal mass ejections and solar energetic particle event characteristics

Papaioannou

Sandberg

Anastasiadis

et al. 2016

J. Space Weather Space Clim.

142

129

View full text Add to dashboard Cite

show abstract

“…These total brightness techniques, originally developed for LASCO instruments on board the Solar and Heliospheric Observatory (SOHO; Domingo et al 1995), have also been extended to the Sun-Earth Connection Coronal and Heliospheric Investigation (SECCHI; Howard et al 2008) instrument suites on board the twin Solar TErrestrial RElations Observatory (STEREO; Kaiser et al 2008) spacecraft. Individually, the white-light imagers on SOHO, STEREO-A, and STEREO-B have been used to develop large online CME catalogs that employ both manual detection methods, such as those used in the SOHO LASCO CME Catalog (Gopalswamy et al 2009), as well as automated detection methods, as used in the Computer Aided CME Tracking software catalog (CACTus; Robbrecht et al 2009) or the Solar Eruptive Event Detection System (SEEDS; Olmedo et al 2008). …”

Section: White-light Imaging Of Cmesmentioning

confidence: 99%

“…Our total intensity white-light analysis in this paper relies primarily on Data for all CMEs that occulted our radio sources appear in numerous CME catalogs; Table 2 summarizes these data from three online catalogs: the SOHO LASCO CME Catalog (Gopalswamy et al 2009), Computer Aided CME Tracking software catalog (CACTus; Robbrecht et al 2009), and the Solar Eruptive Event Detection System (SEEDS; Olmedo et al 2008). In this table, the position angle gives the orientation of the erupting CME and is measured counter-clockwise from Solar North; the angular width gives the approximate angular size of the CME as measured from the sun; the linear velocity and acceleration are determined by fitting a first-order and second-order polynomial, respectively, to the height-time measurements for the event.…”

Section: Properties Of the Occulting Cmesmentioning

confidence: 99%

VLA Measurements of Faraday Rotation through Coronal Mass Ejections

et al. 2017

View full text Add to dashboard Cite

Coronal mass ejections (CMEs) are large-scale eruptions of plasma from the Sun that play an important role in space weather. Faraday rotation (FR) is the rotation of the plane of polarization that results when a linearly polarized signal passes through a magnetized plasma such as a CME and is proportional to the path integral through the plasma of the electron density and the line of sight component of the magnetic field.FR observations of a source near the Sun can provide information on the plasma structure of a CME shortly after launch; however, separating the contribution of the plasma density from the line of sight magnetic field is challenging.We report on simultaneous white-light and radio observations made of three CMEs in August 2012. We made sensitive Very Large Array (VLA) full-polarization observations using 1 − 2 GHz frequencies of a "constellation" of radio sources through the solar corona at heliocentric distances that ranged from 6 − 15R ⊙ . Of the nine sources observed, three were occulted by CMEs: two sources (0842+1835 and 0900+1832) were occulted by a single CME and one source (0843+1547) was occulted by two CMEs. In addition to our radioastronomical observations, which represent one of the first active hunts for CME Faraday rotation since Bird et al. (2007) and Jensen & Russell (2008), as well as previous CME FR observations by Bird et al. (1985).

show abstract

“…This implied that the EUV loops trailed the X-ray source in both space and time, and that the higher energies were located higher than the lower energies (see also Gallagher 2002), constituting the standard Kopp-Pneuman two-ribbon flare configuration. Susino et al (2013) studied EUV/UV data from UVCS, HXR data from RHESSI, and SXR data from GOES of the 2004 July 28 event that developed a partial halo CME with maximum velocity of ∼ 754 km s −1 in the online LASCO CME catalog (Gopalswamy et al 2009) and a small flare. A narrow emission feature in [Fe XVIII] λ974 Å was observed to stand for about 2.5 days by UVCS after the CME crossed the UVCS slit.…”

Section: Identifications Of the Current Sheet In The Solar Eruptive Ementioning

confidence: 99%

Review on Current Sheets in CME Development: Theories and Observations

et al. 2015

View full text Add to dashboard Cite

We introduce how the catastrophe model for solar eruptions predicted the formation and development of the long current sheet (CS) and how the observations were used to recognize the CS at the place where the CS is presumably located. Then, we discuss the direct measurement of the CS region thickness by studying the brightness distribution of the CS region at different wavelengths. The thickness ranges from 10 4 km to about 10 5 km at heights between 0.27 and 1.16 R from the solar surface. But the traditional theory indicates that the CS is as thin as the proton Larmor radius, which is of order tens of meters in the corona. We look into the huge difference in the thickness between observations and theoretical expectations. The possible impacts that affect measurements and results are studied, and physical causes leading to a thick CS region in which reconnection can still occur at a reasonably fast rate are analyzed. Studies in both theories and observations suggest that the difference between the true value and the apparent value of the CS thickness is not significant as long as the CS could be recognised in observations. We review observations that show complex structures and flows inside the CS region and present recent numerical modelling results on some aspects of these structures. Both observations and numerical experiments indicate that the downward reconnection outflows are usually slower than the upward ones in the same eruptive event. Numerical simulations show that the complex structure inside CS and its temporal behavior as a result of turbulence and the Petschek-type slow-mode shock could probably account for the thick CS and fast reconnection. But whether the CS itself is that thick still remains unknown since, for the time being, we cannot measure the electric current directly in that region. We also review the most recent laboratory experiments of reconnection driven by energetic laser beams, and discuss some important topics for future works.

show abstract

The SOHO/LASCO CME Catalog

Cited by 554 publications

References 30 publications

Solar flares, coronal mass ejections and solar energetic particle event characteristics

Solar flares, coronal mass ejections and solar energetic particle event characteristics

VLA Measurements of Faraday Rotation through Coronal Mass Ejections

Review on Current Sheets in CME Development: Theories and Observations

Contact Info

Product

Resources

About