AUTOMATED LASCO CME CATALOG FOR SOLAR CYCLE 23: ARE CMEs SCALE INVARIANT?

Robbrecht, E.; Berghmans, D.; Linden, R. A. M. Van der

doi:10.1088/0004-637x/691/2/1222

Cited by 224 publications

(230 citation statements)

References 43 publications

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“…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%

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VLA Measurements of Faraday Rotation through Coronal Mass Ejections

et al. 2017

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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).

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Section: White-light Imaging Of Cmesmentioning

confidence: 99%

Section: Properties Of the Occulting Cmesmentioning

confidence: 99%

VLA Measurements of Faraday Rotation through Coronal Mass Ejections

et al. 2017

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“…The halo CME is reported in the CACTUS catalog 3 (Robbrecht & Berghmans 2004;Robbrecht et al 2009). However, the reported speed in the LASCO catalog 4 is 1179 km s −1 .…”

Section: Observations Of the Emerging Regionmentioning

confidence: 99%

Supergranular-scale magnetic flux emergence beneath an unstable filament

Palacios

Cid

Guerrero

et al. 2015

A&A

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Aims. Here we report evidence of a large solar filament eruption on 2013, September 29. This smooth eruption, which passed without any previous flare, formed after a two-ribbon flare and a coronal mass ejection towards Earth. The coronal mass ejection generated a moderate geomagnetic storm on 2013, October 2 with very serious localized effects. The whole event passed unnoticed to flarewarning systems. Methods. We have conducted multi-wavelength analyses of the Solar Dynamics Observatory through Atmospheric Imaging Assembly (AIA) and Helioseismic and Magnetic Imager (HMI) data. The AIA data on 304, 193, 211, and 94 Å sample the transition region and the corona, respectively, while HMI provides photospheric magnetograms, continuum, and linear polarization data, in addition to the fully inverted data provided by HMI.Results. This flux emergence happened very close to a filament barb that was very active in mass motion, as seen in 304 Å images. The observed flux emergence exhibited hectogauss values. The flux emergence extent appeared just beneath the filament, and the filament rose during the following hours. The emergence acquired a size of 33 in ∼12 h, about ∼0.16 km s −1 . The rate of signed magnetic flux is around 2 × 10 17 Mx min −1 for each polarity. We have also studied the eruption speed, size, and dynamics. The mean velocity of the rising filament during the ∼40 min previous to the flare is 115 ± 5 km s −1 , and the subsequent acceleration in this period is 0.049 ± 0.001 km s −2 . Conclusions. We have observed a supergranular-sized emergence close to a large filament in the boundary of the active region NOAA11850. Filament dynamics and magnetogram results suggest that the magnetic flux emergence takes place in the photospheric level below the filament. Reconnection occurs underneath the filament between the dipped lines that support the filament and the supergranular emergence. The very smooth ascent is probably caused by this emergence and torus instability may play a fundamental role, which is helped by the emergence.

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“…While the CME observations are relatively easily accessible through a number of sources (e.g. SOHO LASCO CME Catalog 4 , see Gopalswamy et al 2009, and the automated CACTUS CME-detection facility 5 , see Robbrecht et al 2009), energetic photon and radio observations relevant to SEP events have not so far been collected to a single access point. Table 2 presents the EM observations distributed through SEPServer.…”

Section: The Sepserver Projectmentioning

confidence: 99%

The firstSEPServerevent catalogue ~68-MeV solar proton events observed at 1 AU in 1996–2010

Vainio

Валтонен

Heber

et al. 2013

J. Space Weather Space Clim.

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SEPServer is a three-year collaborative project funded by the seventh framework programme (FP7-SPACE) of the European Union. The objective of the project is to provide access to state-of-the-art observations and analysis tools for the scientific community on solar energetic particle (SEP) events and related electromagnetic (EM) emissions. The project will eventually lead to better understanding of the particle acceleration and transport processes at the Sun and in the inner heliosphere. These processes lead to SEP events that form one of the key elements of space weather. In this paper we present the first results from the systematic analysis work performed on the following datasets: SOHO/ERNE, SOHO/EPHIN, ACE/EPAM, Wind/WAVES and GOES X-rays. A catalogue of SEP events at 1 AU, with complete coverage over solar cycle 23, based on high-energy (~68-MeV) protons from SOHO/ERNE and electron recordings of the events by SOHO/EPHIN and ACE/EPAM are presented. A total of 115 energetic particle events have been identified and analysed using velocity dispersion analysis (VDA) for protons and time-shifting analysis (TSA) for electrons and protons in order to infer the SEP release times at the Sun. EM observations during the times of the SEP event onset have been gathered and compared to the release time estimates of particles. Data from those events that occurred during the European day-time, i.e., those that also have observations from ground-based observatories included in SEPServer, are listed and a preliminary analysis of their associations is presented. We find that VDA results for protons can be a useful tool for the analysis of proton release times, but if the derived proton path length is out of a range of 1 AU < s [ 3 AU, the result of the analysis may be compromised, as indicated by the anti-correlation of the derived path length and release time delay from the associated X-ray flare. The average path length derived from VDA is about 1.9 times the nominal length of the spiral magnetic field line. This implies that the path length of first-arriving MeV to deka-MeV protons is affected by interplanetary scattering. TSA of near-relativistic electrons results in a release time that shows significant scatter with respect to the EM emissions but with a trend of being delayed more with increasing distance between the flare and the nominal footpoint of the Earth-connected field line.

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AUTOMATED LASCO CME CATALOG FOR SOLAR CYCLE 23: ARE CMEs SCALE INVARIANT?

Cited by 224 publications

References 43 publications

VLA Measurements of Faraday Rotation through Coronal Mass Ejections

VLA Measurements of Faraday Rotation through Coronal Mass Ejections

Supergranular-scale magnetic flux emergence beneath an unstable filament

The firstSEPServerevent catalogue ~68-MeV solar proton events observed at 1 AU in 1996–2010

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