Extremely high speed solar wind: 29–30 October 2003

By R. Skoug, J. Gosling, J. Steinberg, David John McComas, Charles W. Smith, N. Ness, Qiang Hu, L. Burlaga. 2004

218 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/37702ca7b674936e4dc6656de9fe52f70b6ad65c

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In Astronomy and Astrophysics

Citations in the corpus

CME interactions with coronal holes and their interplanetary consequences (2009, result): “Boundaries differ in published works [ Skoug et al. , 2004; Malandraki et al. , 2005].”
Coronal mass ejections and other extreme characteristics of the 2003 October–November solar eruptions (2005, background): “At 1 AU, these shocks continued to be driven by the IP counterparts of CMEs [see Skoug et al., 2004; Tokumaru et al., 2005].”
Large-scale traveling ionospheric disturbances observed by GPS total electron content during the magnetic storm of 29-30 October 2003 (2007, background): “3.1. Geomagnetic Activity [19] The super geomagnetic storm during 29–30 October 2003 was originally caused by two consecutive, extremely huge Sun flare events [ Skoug et al., 2004; Zhao et al., 2005].”
Proton, helium, and electron spectra during the large solar particle events of October-November 2003 (2005, background): “For example, in event 2 the solar wind speed exceeded 1850 km/s following the arrival of the shock on 29 October 2003 and it remained >1000 km/s for most of the following 2 days [ Skoug et al., 2004 ].”
Dayside global ionospheric response to the major interplanetary events of October 29–30, 2003 “Halloween Storms” (2005, methodology): “The resultant time series of average vertical TEC versus UT is plotted along with the computed interplanetary electric field (IEF), derived from the product Vx Bz (GSM coordinates) measured by the plasma and magnetic field instruments onboard the ACE spacecraft [ Skoug et al., 2004 ].”
An overview of the impulsive geomagnetic field disturbances and power grid impacts associated with the violent Sun‐Earth connection events of 29–31 October 2003 and a comparative evaluation with other contemporary storms (2005, background): “[11] Because of the extremely high speed of the solar wind (2000 km/sec) [ Skoug et al., 2004 ], a considerable amount of buffeting is suspected to have occurred to the Earth’s magnetosphere, which presumably would be especially pronounced in the morning dayside sector from the Kelvin-Helmholtz shea”
The 1859 Solar–Terrestrial Disturbance And the Current Limits of Extreme Space Weather Activity (2004, background): “Solar wind measurements for the three modern events on the list (4 August 1972 (Vaisberg and Zastenker, 1976; d’Uston et al., 1977) and 28 and 29 October 2003 (Skoug et al., 2004)) indicate peak speeds ∼ 2000 km s−1.”
Three-dimensional MHD Simulation of the 2003 October 28 Coronal Mass Ejection: Comparison with LASCO Coronagraph Observations (2008, methodology): “The simulated solar wind velocity at the Earth increases from about 350 km s−1 to 550 km s−1, which is a good approximation to the solar wind conditions preceding the arrival of the October 28 CME as observed by the ACE satellite (Skoug et al. 2004; Zurbuchen 2004).”
Interplanetary conditions leading to superintense geomagnetic storms (Dst ≤ −250 nT) during solar cycle 23 (2008, methodology): “For the November 2001 and October 2003 events, we used the reprocessed plasma data presented by Skoug et al. [2004] , Tsurutani et al. [2004], and Mannucci et al. [2005].”