Composition of quasi‐stationary solar wind flows from Ulysses/Solar Wind Ion Composition Spectrometer

By R. Steiger, N. Schwadron, L. Fisk, J. Geiss, G. Gloeckler, S. Hefti, B. Wilken, R. Wimmer-Schweingruber, T. Zurbuchen. 2000

409 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/7b2d95a6a6fe670b083fd298d57c6c652e6a4536

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Citations in the corpus

• Self-consistent Coronal Heating and Solar Wind Acceleration from Anisotropic Magnetohydrodynamic Turbulence (2007, methodology): “The data points, obtained from the online database of T. Zurbuchen and R. von Steiger (see also von Steiger et al. 2000), were grouped in sequential bins of wind speed of size 25 km s−1, and the mean and standard deviation of the ionization ratio in each bin were computed.”
• Mercury’s Weather-Beaten Surface: Understanding Mercury in the Context of Lunar and Asteroidal Space Weathering Studies (2014, background): “Energies ranging up to 5 keV/nucleon are dominated by solar wind; the expanding corona of the slow solar wind nominally consists of a quasi-neutral plasma of ∼96 % protons (H+) and electrons, as well as ∼4 % alpha particles (He2+) and <0.1 % heavy ions (von Steiger et al. 2000).”
• The Two Sources of Solar Energetic Particles (2012, methodology): “Coronal abundances are also measured with X-ray (e.g. Fludra and Schmelz 1999; Landi, Feldman, and Dochek 2007) and γ-ray (Ramaty and Murphy 1987; Ramaty et al. 1995) lines and in the solar wind (von Steiger et al. 2000, Gloeckler and Geiss 2007).”
• X-rays from solar system objects (2007, background): “Minor, heavy ions account for about 0.1% of the solar wind and exist in highly charged states such as O7+, O6+, C6+, C5+, N6+, Ne8+, Si9+, and Fe12+ (Schwadron and Cravens, 2000; von Steiger et al., 2000).”
• The FIP and Inverse FIP Effects in Solar and Stellar Coronae (2015, methodology): “Observations with Ulysses, the first mission to fly over the solar polar regions (Wenzel et al., 1992) revealed FIP fractionation varying with wind speed (Zurbuchen et al., 1999; von Steiger et al., 2000).”
• Solar cycle changes in coronal holes and space weather cycles (2002, background): “These include intervals of observed complex current sheet structures [e.g., Crooker et al., 1993] and composition variations [e.g., von Steiger, 2000], suggesting contributions from a number of regions with different degrees of active region involvement, unlike the polar region streams that are…”
• Heavy-Ion Elemental Abundances in Large Solar Energetic Particle Events and Their Implications for the Seed Population (2006, methodology): “In order to identify the source populations for LSEP events, we compare the heavy-ion abundances with those measured in the fast and slow solar wind (von Steiger et al. 2000) and in particle populations accelerated near the Sun (Reames 1995a;Mason et al. 2004) and in IP space (Desai et al. 2003).”
• The solar wind composition throughout the solar cycle: A continuum of dynamic states (2002, background): “Note that there are large systematic abundance variations, particularly in slow solar wind, that by far exceed these statistical error bars, as discussed elsewhere [e.g., Zurbuchen et al., 2000; von Steiger et al., 2000].”
• The Solar Probe Plus Mission: Humanity’s First Visit to Our Star (2016, background): “The slow solar wind has, however, distinctive compositional properties (Geiss et al. 1995; von Steiger et al. 2000; Ko et al. 2006) that argue for a different origin of this plasma outside coronal holes.”
• Origins of the Ambient Solar Wind: Implications for Space Weather (2017, methodology): “Figure 2 shows data from the Ulysses SWICS (Solar Wind Ion Composition Spectrometer) instrument final archive to illustrate how the traditional O+7/O+6 charge-state ratio varies as a function of solar wind speed (Gloeckler et al. 1992; von Steiger et al. 2000).”
• Global distribution of the solar wind during solar cycle 23: ACE observations (2009, background): “[4] There are also samples of the non-transient solar wind that have higher O7+/O6+ ratios, and thus higher freeze-in temperatures [von Steiger et al., 2000].”
• The Behavior of the Open Magnetic Field of the Sun (2001, background): “Fast solar wind shows a much smaller FIP enhancement (Geiss, Gloeckler, & von Steigner 1995 ; von Steiger et al. 2000).”