Physics of the Solar Corona: An Introduction with Problems and Solutions

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Hinode observations of transverse waves with flows in coronal loops (2008, methodology): “…al. 1999; Nakariakov & Ofman 2001; Ofman 2002; De Moortel et al. 2002; Ofman & Wang 2002; Ofman & Thompson 2002; Verwichte et al. 2004; Wang & Solanki 2004; Aschwanden 2005), with recent advances (e.g., Ofman 2007; Wang et al. 2007; Van Doorsselaere et al. 2007; Ballai 2007; Arregui et al. 2007).”
The magnetic field in the solar atmosphere (2014, background): “…heights thus depend, besides on the distance between neighbouring magnetic features, on the temperature difference between the magnetic field structures and their surroundings, causing successively lower canopy heights for increasing temperature differences (see chapter 5 of Aschwanden (2005)).”
NO TRACE LEFT BEHIND: STEREO OBSERVATION OF A CORONAL MASS EJECTION WITHOUT LOW CORONAL SIGNATURES (2009, methodology): “For ne(r), we used the density profiles of Baumbach-Allen (Aschwanden 2005; Gibson et al. 1999; Guhathakurta et al. 1996).”
Extreme states of matter on Earth and in space (2009, unknown): “Magnetohydrodynamic phenomena on the Sun have been studied, of course, most thoroughly [242].”
Deducing Electron Properties from Hard X-ray Observations (2011, methodology): “To account for elements heavier than hydrogen, the Compton cross-section is multiplied by an effective mean atomic number Z = 1.2 (e.g., Aschwanden 2005, for element abundances).”