Coronal mass ejections and other extreme characteristics of the 2003 October–November solar eruptions

By Nat Gopalswamy, S. Yashiro, Yijin Liu, G. Michalek, A. Vourlidas, M. Kaiser, R. Howard. 2005

186 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/5d0693e5055e0db95d9d7bcf089bed2a029308b9

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

Citations in the corpus

Geoeffectiveness of halo coronal mass ejections (2007, background): “Occasionally, the flux rope axes may be highly inclined to the ecliptic plane and cause either very intense storms [Gopalswamy et al., 2005a] or no storm at all [Yurchyshyn et al., 2001] depending on which way the axial field is pointed.”
Space Weather: The Solar Perspective (2006, background): “…of these extraordinary Halloween events and their effects were assembled in special editions of Geophysical Research Letters and Journal of Geophysical Research (see http: //www.agu.org/journals/ss/VIOLCONN1/ and were reviewed by Veselovsky et al. (2004), (see also Gopalswamy et al., 2005b).”
Coronal mass ejections of solar cycle 23 (2006, background): “The solid curve is the empirical shock arrival (ESA) model, which relates the Sun–Earth transit time (T in hours) to the CME speed (V km s−1) by the formula, T = abV + c, where a = 151.002, b = 0.998625, and c = 11.5981 (Gopalswamy et al. 2005a).”
Properties of Ground Level Enhancement Events and the Associated Solar Eruptions During Solar Cycle 23 (2012, methodology): “Type II bursts with emission components from metric to kilometric wavelengths indicate that the driving CMEs are of the highest kinetic energy (Gopalswamy et al. 2005b).”
CME interactions with coronal holes and their interplanetary consequences (2009, background): “Interestingly, the same region (AR 0501) produced another halo CME two days earlier (2003 November 18) when it was at S01E33, resulting in a shock with driver (a magnetic cloud) at Earth and caused the largest geomagnetic storm of cycle 23 [see Gopalswamy et al., 2005a].”
Global Properties of Solar Flares (2011, methodology): “We illustrate this point in Figure 20, based on data compiled by Gopalswamy et al. (2005).”
Proton, helium, and electron spectra during the large solar particle events of October-November 2003 (2005, background): “…of November was marked by some of the most intense solar activity in the history of the space age, including 43 coronal mass ejections (CMEs) [see Gopalswamy et al., 2005], eight X-class flares, some of the largest solar particle events of this solar cycle, and two of the largest geomagnetic…”
The 1859 space weather event revisited: limits of extreme activity (2013, background): “occurred during the " Halloween " event sequence of flares (Gopalswamy et al. 2005).”
Composition changes after the "Halloween" solar proton event: the High Energy Particle Precipitation in the Atmosphere (HEPPA) model versus MIPAS data intercomparison study (2011, methodology): “A more detailed description of the October–November 2003 SPE period is given in Gopalswamy et al. (2005). The ionization rates should provide a similar forcing for all models, therefore the original data set has been adopted to every model grid.”
The SOHO/LASCO CME Catalog (2009, background): “CMEs can also be deflected by other CMEs and by nearby coronal holes (Gopalswamy et al. 2005a).”
Type II radio bursts and energetic solar eruptions (2003, methodology): “SOHO observations have demonstrated that the propagation of CMEs is severely affected by the presence of nearby coronal holes [Gopalswamy et al., 2004, 2005a].”