Solar wind observations over Ulysses' first full polar orbit

By David John McComas, B. Barraclough, H. Funsten, J. Gosling, E. Santiago-Muñoz, R. Skoug, B. Goldstein, M. Neugebauer, Pete Riley, A. Balogh. 2000

418 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/de3ea3b24dee1dbf50dd84ae96f12d58b000d2aa

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In Astronomy and Astrophysics

Citations in the corpus

Polarization of Prompt Gamma-Ray Burst Emission: Evidence for Electromagnetically Dominated Outflow (2003, background): “There is a good precedent for this behavior in Ulysses observations of the quiet solar wind (McComas et al. 2000) which reveal that, despite the complexity of the measured surface magnetic field, the field in the solar wind quickly rearranges to form a good approximation to a Parker (1960) spiral.”
Solar cycle changes in coronal holes and space weather cycles (2002, background): “…low-latitude solar wind observed in interplanetary scintillation (IPS) measurements [e.g., Asai et al., 1998; Kojima et al., 1999] and by Ulysses [McComas et al., 2000; von Steiger et al., 2000], though it is likely that there is also a contribution to low-latitude solar wind from weak coronal…”
The Magnetic Landscape of the Sun's Polar Region (2008, background): “These values exhibit little variation with heliolatitude (McComas et al. 2000).”
INCORPORATING KINETIC PHYSICS INTO A TWO-FLUID SOLAR-WIND MODEL WITH TEMPERATURE ANISOTROPY AND LOW-FREQUENCY ALFVÉN-WAVE TURBULENCE (2011, background): “The filled circle is the mean proton densityn= 2.7±0.86 cm−3 at heliographic latitudes> 36◦ measured during Ulysses’ first polar orbit, scaled tor = 1 AU (McComas et al. 2000).Middle panel:Important time scales in our steady-state numerical solution.”
Weaker solar wind from the polar coronal holes and the whole Sun (2008, background): “The wind is comprised of essentially two types: 1) fast, tenuous and relatively homogeneous solar wind at high heliolatitudes emanating from large PCHs that persisted throughout most of the SC and 2) slower, denser, and highly variable wind at lower latitudes [e.g., McComas et al., 1998a, 2000].”
Bulk properties of the slow and fast solar wind and interplanetary coronal mass ejections measured by Ulysses: Three polar orbits of observations (2009, background): “In the case of the fast wind, this deviation is attributed to the presence of Alfvén waves at high latitudes [Smith et al., 1995; McComas et al., 2000].”
Heating of the low‐latitude solar wind by dissipation of turbulent magnetic fluctuations (2001, background): “High-speed winds at 1 AU are observed to be generally hotter than the surrounding plasma Barnes, 1979] and Ulysses observations at high latitudes and in high-speed wind show similarly consistent high temperatures McComas et al., 2000].”
Electron and proton heating by solar wind turbulence (2009, neutral): “S R ] 2 3 Ju l 2 00 9 JOURNAL OF GEOPHYSICAL RESEARCH, VOL. ???, XXXX, DOI:10.1029/,”
A MODEL FOR THE SOURCES OF THE SLOW SOLAR WIND (2010, background): “More important, the slow wind appears to be inherently non-steady when compared to the fast wind (e.g., Bame et al. 1977; Schwenn 1990; Gosling 1997; McComas et al. 2000).”
The solar wind composition throughout the solar cycle: A continuum of dynamic states (2002, background): “[6] The dramatic differences of V from solar minimum to maximum have been described byMcComas et al. [2000b]. During solar minimum a large part of the heliosphere is dominated by solar wind emerging from stable polar coronal holes.”