Ultraviolet spectroscopy of the extended solar corona

By J. Kohl, G. Noci, S. Cranmer, J. C. Raymond. 2006

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In Astronomy and Astrophysics

Citations in the corpus

Solar Orbiter (2012, background): “…of the very high temperatures and anisotropies of coronal heavy ions suggest that other processes such as magnetic mirror and wave–particle interactions should also contribute strongly to the expansion of the fast wind (Li et al., 1998; Kohl et al. 1997, 1998, 2006; Dodero et al., 1998).”
Self-consistent Coronal Heating and Solar Wind Acceleration from Anisotropic Magnetohydrodynamic Turbulence (2007, background): “The original motivation for this work was to understand the preferential ion heating and acceleration in the corona revealed by the UVCS (Ultraviolet Coronagraph Spectrom- eter) instrument onSOHO (Kohl et al. 1995, 1997, 2006).”
EMPIRICAL CONSTRAINTS ON PROTON AND ELECTRON HEATING IN THE FAST SOLAR WIND (2009, background): “The observational consensus since the late 1990s has been that coronal holes undergo preferential proton heating in a similar sense as high-speed wind streams in the heliosphere (see, e.g., Kohl et al. 1997, 1998, 2006; Wilhelm et al. 2007).”
A MODEL FOR THE SOURCES OF THE SLOW SOLAR WIND (2010, background): “The proton and ion temperatures measured in situ and in coronal holes by UVCS, for example, (e.g., Kohl et al. 2006) show the opposite trend in that the ion temperatures are substantially higher in the fast wind than in the slow (Marsch 2006).”
Slow Solar Wind: Observations and Modeling (2016, unknown): “UVCS spectroscopic observations have significantly contributed to our understanding of streamers and slow wind since the beginning of the SOHO mission (see also Antonucci 2006; Kohl et al. 2006 for reviews of UVCS results).”
Coronal Mass Ejections: Observations (2012, background): “The UVCS instrument, in particular, which overlaps the same height range as LASCO C2, has provided a wealth of data on the evolution of hundreds of CMEs (see review by Kohl et al., 2006).”
A Model of Turbulence in Magnetized Plasmas: Implications for the Dissipation Range in the Solar Wind (2007, background): “o yield the observed minority ion temperatures higher than proton temperatures Tion > Tp and large ion and proton temperature anisotropies T⊥ ≫ Tk [Kohl et al., 1997, 1998; Antonucci et al., 2000; Kohl et al., 2006]. In the spirit of a long line of previous investigations [Hollweg, 1986; Isenberg”
Origins of the Ambient Solar Wind: Implications for Space Weather (2017, methodology): “Figure 5 summarizes the evidence found by the Ultraviolet Coronagraph Spectrometer (UVCS) instrument on the Solar and Heliospheric Observatory (SOHO) for preferential ion heating and acceleration above coronal holes (see, e.g., Kohl et al. 2006).”