Improvement in the prediction of solar wind conditions using near‐real time solar magnetic field updates

By Charles N. Arge, V. Pizzo. 2000

685 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/e3a39233ffe8c92e33f5adfb2fbe449ce681a6bf

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Citations in the corpus

NUMERICAL SIMULATION OF AN EUV CORONAL WAVE BASED ON THE 2009 FEBRUARY 13 CME EVENT OBSERVED BY STEREO (2009, methodology): “Second, this potential field distribution is used to calculate the distribution of the terminal solar wind speed, uwsa as a function of the flux tube expansion factor, fs, based on the Wang-Sheeley-Arge (WSA) model (Wang & Sheeley 1990; Arge & Pizzo 2000).”
Flux tube texture of the solar wind: Strands of the magnetic carpet at 1 AU?: FLUX TUBE TEXTURE OF SOLAR WIND (2008, methodology): “[25] A proper mapping of flux tube measurements from 1 AU to the Sun would utilize magnetogram-based mapping techniques that can account for mapping to the off- equatorial regions and for the magnetic-flux expansion factor in the corona [Arge and Pizzo, 2000;Arge et al., 2003;Owens et al., 2005].”
Slow Solar Wind: Observations and Modeling (2016, positive): “Its empirical prediction of the solar wind speed at 1 AU provides a certain level of support (Wang and Sheeley 1990; Arge and Pizzo 2000).”
ON THE WEAKENING OF THE POLAR MAGNETIC FIELDS DURING SOLAR CYCLE 23 (2009, background): “…of coronal holes displayed in Figure 10; also plotted are the source-surface field and the solar wind-speed distribution at 1 AU, derived from the inverse correlation between wind speed and flux-tube expansion factor (see, e.g., Wang & Sheeley 1990, 2006; Arge & Pizzo 2000; Luhmann et al. 2009).”
A major solar eruptive event in July 2012: Defining extreme space weather scenarios (2013, methodology): “The propagation of this CME was modeled in near real time by the NASA Goddard Space Weather Research Center at the Community Coordinated Modeling Center using the Wang-Sheeley-Arge (WSA) ENLIL+Cone model [see Arge and Pizzo, 2000; Odstrcil et al., 2004].”
Stellar winds on the main-sequence - II. The evolution of rotation and winds (2015, background): “The spatial distribution of slow and fast wind is closely associated with the structure of the solar magnetic field (Wang & Sheeley 1990; Arge & Pizzo 2000).”
Origins of the Ambient Solar Wind: Implications for Space Weather (2017, methodology): “Further refinement in the exact functional dependence of u on f and other parameters has led to the widely-used Wang-Sheeley-Arge (WSA) empirical model (see also Arge and Pizzo 2000; Arge et al. 2003; Wang and Sheeley 2006; Riley et al. 2015).”
Ultraviolet spectroscopy of the extended solar corona (2006, background): “Levine et al. (1977) and Wang & Sheeley (1990) found that the asymptotic wind speed is inversely correlated with the amount of transverse flux-tube expansion between the solar surface and a reference point in the mid-corona (Arge & Pizzo 2000; Poduval & Zhao 2004).”
STEREO IMPACT Investigation Goals, Measurements, and Data Products Overview (2008, positive): “…at NOAA SEC to make predictions of the solar wind speed and interplanetary field polarity based on the Wang/Sheeley/Arge semi-empirical approach (Arge and Pizzo 2000; at http://sec.noaa.gov/wsa/), at the LMSAL Solar Soft site for coronal holes and solar wind source mapping…”
Solar cycle changes in coronal holes and space weather cycles (2002, methodology): “The model velocities (in kilometers per second) in the center panel are computed for the low-latitude source surface using the Wang and Sheeley [1990b] approach but with the velocity dependence on flux tube expansion factor from Arge and Pizzo [2000]. Although the solar cycle is less evident in the ”