The solar wind composition throughout the solar cycle: A continuum of dynamic states

By T. Zurbuchen, L. Fisk, G. Gloeckler, R. Steiger. 2002

160 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/4499fc670860b4a13046a3b9161849b00bf73fb8

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In Astronomy and Astrophysics

Citations in the corpus

Mercury’s Weather-Beaten Surface: Understanding Mercury in the Context of Lunar and Asteroidal Space Weathering Studies (2014, background): “For example, fast solar wind has a substantially lower oxygen charge-state ratio (O7+/O6+ = 0.01) than slow wind (O7+/O6+ = 0.2) or CMEs (O7+/O6+ > 1) (Zurbuchen et al. 2002; Gloeckler et al. 2003).”
The FIP and Inverse FIP Effects in Solar and Stellar Coronae (2015, background): “The model results are compared with observations taken from the literature; (a) Zurbuchen et al. (2002), given relative to O, (b) Bochsler (2007a), relative to O, (c) Giammanco et al. (2007, 2008), relative to H, (d) Bryans et al. (2009), given relative to the mean of O, Ne and Ar and, (e) Phillips…”
A MODEL FOR THE SOURCES OF THE SLOW SOLAR WIND (2010, background): “The data show that the slow wind has a higher freeze-in temperature (≥ 1.5 × 106K) than the fast wind (≤ 1.2 × 106K) (von Steiger et al. 1997, 2001; Zurbuchen et al. 1999, 2002).”
The Wide-Field Imager for Solar Probe Plus (WISPR) (2014, background): “Reconnection between open and closed magnetic field lines (Antiochos et al. 2007; interchange reconnection: Crooker et al. 2004; Zurbuchen et al. 2002), between closed magnetic fields lines (generating helical fields) and between open field lines of opposite polarities (Einaudi et al. 1999; Wang et…”
The Solar Probe Plus Mission: Humanity’s First Visit to Our Star (2016, background): “This has been suggested to explain the inverse correlation between wind speed and both electron temperature (Gloeckler et al. 2003) and compositional enhancement of low-FIP (First Ionization Potential) elements (Zurbuchen et al. 2002).”
Self-consistent Coronal Heating and Solar Wind Acceleration from Anisotropic Magnetohydrodynamic Turbulence (2007, background): “Specifically, the ratio of number densities of O7+ to O6+ is often used to aid in the identification of fast and slow wind streams (e.g., Zurbuchen et al. 2002).”
Anisotropy in Fast and Slow Solar Wind Fluctuations (2005, background): “The relative abundance of charge states of heavy ions is different in fast and slow wind: low values of charge state are generally associated with higher speed streams (e.g., Zurbuchen et al. 2002 and references therein).”