Weaker solar wind from the polar coronal holes and the whole Sun

By David John McComas, R. Ebert, H. Elliott, B. Goldstein, J. Gosling, N. Schwadron, R. Skoug. 2008

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View Paper: https://www.semanticscholar.org/paper/b6e68ad6c2df06c4cd71b9b82e5931affa1af7ec

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In Astronomy and Astrophysics

Citations in the corpus

Origins of the Ambient Solar Wind: Implications for Space Weather (2017, background): “…when it left the ecliptic plane and showed that the fast wind is ubiquitous over large polar coronal holes, which (1) persist over more than half of each solar cycle, and (2) expand out to fill the majority of the heliospheric volume (Goldstein et al. 1996; Marsden 2001; McComas et al. 2008).”
RECORD-SETTING COSMIC-RAY INTENSITIES IN 2009 AND 2010 (2010, background): “…2010 (Figures 1(b) and (c)), and the Sun entered an unfamiliar state characterized by much weaker polar and interplanetary magnetic fields (IMFs; Smith & Balogh 2008; Lee et al. 2009; Figure 1(d)) and by greatly reduced solar-wind density and dynamic pressure (McComas et al. 2008; Figure 1(f)).”
The Heliospheric Magnetic Field (2013, background): “This has been accompanied by a significant reduction in the solar wind momentum flux (McComas et al., 2008).”
Global MHD Modeling of the Solar Corona and Inner Heliosphere for the Whole Heliosphere Interval (2008, background): “Instead, the similar speeds are consistent with the Ulysses results that while the density dropped between WSM and WHI, the speed remained constant (McComas et al., 2008).”
Solar Orbiter (2012, background): “…fast solar wind found by Ulysses during its first two orbits, although the dramatic decrease in mass flux over the present cycle points also to a decreased efficiency of coronal heating and therefore to its dependence on the solar magnetic field (McComas et al., 2008; Schwadron and McComas, 2008).”
ON THE WEAKENING OF THE POLAR MAGNETIC FIELDS DURING SOLAR CYCLE 23 (2009, methodology): “From an analysis of Ulysses plasma measurements taken during 2006–2008, McComas et al. (2008) found that the polar-hole wind was ∼17% less dense and ∼14% cooler than during the previous solar minimum; the wind speed vU was only ∼3% lower, but the proton flux density nUvU was ∼20% smaller.”
Anthropogenic and Natural Radiative Forcing (2014, background): “However, SC 23 showed an activity decline not previously seen in the satellite era (McComas et al., 2008; Smith and Balogh, 2008; Russell et al., 2010).”
INTERSTELLAR GAS FLOW PARAMETERS DERIVED FROM INTERSTELLAR BOUNDARY EXPLORER-Lo OBSERVATIONS IN 2009 AND 2010: ANALYTICAL ANALYSIS (2012, background): “This very close match in the maximum observed rate is most likely due to the extended solar minimum over the past few years (e.g., McComas et al. 2008), with the He ionization rate only up by ≈10% in 2009 over 2008 (Bzowski et al. 2012).”
A MODEL FOR THE SOURCES OF THE SLOW SOLAR WIND (2010, background): “In terms of its origins at the Sun, the best understood is the fast wind, which typically exhibits speeds in excess of 600 km/s at 1 AU and beyond (e.g., McComas et al. 2008).”
SEPARATION OF THE INTERSTELLAR BOUNDARY EXPLORER RIBBON FROM GLOBALLY DISTRIBUTED ENERGETIC NEUTRAL ATOM FLUX (2011, background): “This reduction in flux from the first to the second six-month map appears qualitatively consistent with a known reduction in the solar wind flux in the recent solar minimum (McComas et al. 2008; Schwadron & McComas 2008).”
Slow Solar Wind: Observations and Modeling (2016, positive): “The SSW tends to encompass the heliospheric current sheet (HCS), but it extends up to 30◦ in heliocentric latitude (McComas et al. 2008; Wang et al. 2000).”