A catalog of white light coronal mass ejections observed by the SOHO spacecraft

By S. Yashiro, Nat Gopalswamy, G. Michałek, O. S. Cyr, S. Plunkett, N. Rich, R. Howard. 2004

932 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/194c61f9a6b62f72eac76cabc0e00cd4997fcdd2

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In Astronomy and Astrophysics

1. M. Temmer
2. Nat Gopalswamy
3. B. Vršnak
4. D. Webb
5. T. Howard
6. S. Yashiro
7. R. Schwenn
8. N. Lugaz

Citations in the corpus

• Ultraviolet spectroscopy of the extended solar corona (2006, background): “Coronal mass ejections (CMEs) are dramatic eruptions of prominence and coronal plasma at speeds ranging from 100 to 2500 km s , and typical masses are 10 to 10 g (e.g., Sheeley et al. 1999; Vourlidas et al. 2000; Yashiro et al. 2004).”
• Space Weather: The Solar Perspective (2006, methodology): “Right panel: Time-height diagram for the light bulb CME, as derived by Yashiro et al. (2004), see http://cdaw.”
• DIFFERENTIAL EMISSION MEASURE ANALYSIS OF MULTIPLE STRUCTURAL COMPONENTS OF CORONAL MASS EJECTIONS IN THE INNER CORONA (2012, background): “Coronal mass ejections (CMEs) are perhaps the most spectacular form of solar activity, which expel large quantities of plasma (order of ∼1010 to ∼1013 kg) at a speed of hundreds of km s−1 with the fastest ones over 3000 km s−1 (Yashiro et al. 2004; Chen 2011).”
• Near-earth solar wind flows and related geomagnetic activity during more than four solar cycles (1963-2011) (2012, background): “The results indicate that the percentage of the time when the CME-associated flows are present tends to follow the solar activity/sunspot cycle, as would be expected given that the CME rate at the Sun follows the activity cycle (Webb & Howard 1994; Yashiro et al. 2004; Robbrecht et al. 2009).”
• A Statistical Study of Main and Residual Accelerations of Coronal Mass Ejections (2006, background): “Further, the statistical distribution of CME velocity of thousands of events consistently showed a continuous distribution with a single peak (Howard et al. 1985; Hundhausen et al. 1994; St. Cyr et al. 2000; Yashiro et al. 2004; Yurchyshyn et al. 2005).”
• The Heliospheric Magnetic Field (2013, methodology): “CMEs become more frequent and cover a greater latitudinal span (e.g., St Cyr et al., 2000; Yashiro et al., 2004).”
• Processes that Promote and Deplete the Exosphere of Mercury (2007, background): “Compared to the general population of CMEs, halos have much higher average speeds of 1,004 km/s (Yashiro et al. 2004).”
• Ensemble Modeling of CMEs Using the WSA–ENLIL+Cone Model (2015, background): “The third column lists (for 2013) the 2nd order plane-of-the-sky (POS) speed at 20 R⊙ reported in the SOHO LASCO CDAW CME catalog(4) (Yashiro et al., 2004; Gopalswamy et al., 2009).”
• A Model for Spectral and Compositional Variability at High Energies in Large, Gradual Solar Particle Events (2006, background): “We gratefully acknowledge data provided by the ACE Science Center, NSSDC, NOAA, and the SOHO LASCO CME catalog, which is generated and maintained by NASA and TheCatholicUniversity ofAmerica in cooperationwith theNaval Research Laboratory.”
• > 25 MeV Proton Events Observed by the High Energy Telescopes on the STEREO A and B Spacecraft and/or at Earth During the First ∼ Seven Years of the STEREO Mission (2014, methodology): “…CME widths and speeds from the Catholic University of America/Goddard Space Flight Center CDAW CME catalog (http: //cdaw.gsfc.nasa.gov/CME list/; Yashiro et al., 2004) compiled from observations made by the LASCO coronagraphs on SOHO, while recognizing that SOHO may not be the best spacecraft…”
• A study of solar energetic particle events of 1997–2006: Their composition and associations (2010, methodology): “[14] Associated CMEs were identified using the Catholic University of America (CUA) Large Angle and Spectrometric Coronagraph (LASCO) catalog [Yashiro et al., 2004].”
• COMPREHENSIVE ANALYSIS OF CORONAL MASS EJECTION MASS AND ENERGY PROPERTIES OVER A FULL SOLAR CYCLE (2010, methodology): “This resource has been used extensively to study various CME properties (St. Cyr et al. 2000; Yashiro et al. 2004; Gopalswamy et al. 2009).”
• Visibility of coronal mass ejections as a function of flare location and intensity (2005, methodology): “[9] We used the SOHO/LASCO CME Catalog (http:// cdaw.gsfc.nasa.gov/) [Yashiro et al., 2004] to investigate the CME associations.”
• Automatic Detection and Tracking of Coronal Mass Ejections in Coronagraph Time Series (2008, methodology): “The mean and median of the angular width for normal CMEs within the distribution were found to be 40◦ and 34◦, respectively; normal CMEs are the ones that are found to have an angular width greater than 20◦ and less than 120◦ (Yashiro et al., 2004).”
• Solar wind drivers of geomagnetic storms during more than four solar cycles (2012, background): “The three flow types are: (1) Corotating high-speed streams (typically with solar wind speed Vsw > ~450 km s 1) (Belcher & Davis 1971) that originate in coronal holes at the Sun (Krieger et al. 1973; Zirker 1977), and the associated corotating interaction regions; (2) Slower, interstream solar wind,”
• Type II radio bursts and energetic solar eruptions (2003, background): “[5] Halo and partial halo CMEs observed by SOHO during cycle 23 are faster and wider than the average CME [Yashiro et al., 2004; Gopalswamy, 2004b].”