Modeling of Coronal EUV Loops Observed with TRACE. I. Hydrostatic Solutions with Nonuniform Heating

By Markus J. Aschwanden, C. Schrijver, D. M. Alexander. 2001

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In Astronomy and Astrophysics

Citations in the corpus

Nanoflare Heating of the Corona Revisited (2004, background): “This also suggests that the more general overdensity of cooler loops seen by TRACE (e.g., Aschwanden et al. 2001; Warren & Winebarger 2003; Winebarger et al. 2003a) is a natural consequence of a cyclical heating-cooling of the loops, although verification of this claim in the context of the…”
Are Magnetic Dips Necessary for Prominence Formation? (2001, background): “…that solar prominences are straightforward consequences of just two observed properties of the Sun’s corona: heating concentrated near the chromosphere on scales on the order of 10 Mm (Aschwanden et al. 2000, 2001) and magnetic shear localized near neutral lines (e.g., Schmieder et al. 1996).”
Plasma Beta above a Solar Active Region: Rethinking the Paradigm (2001, background): “…of the gray shadowed region is an extension of a factor of 10 above our pressure model in the chromosphere–corona to account for over pressures of non-steady-state loops (Aschwanden, Schrijver, and Alexander, 2001; Aschwanden et al., 1999) and high-temperature SXT loops (Yoshida and Tsuneta, 1996).”
On Solving the Coronal Heating Problem (2005, background): “…cool (T < 0.2 MK) loops (Antiochos and Noci, 1986; Feldman, Widing, and Warren, 1999, 2000; Peter, 2001), and in the lower legs of warm and hot loops (Aschwanden, Schrijver, and Alexander, 2001), but higher altitude reconnection must play an important, if not dominant, role in heating the corona.”
Effect of longitudinal magnetic and density inhomogeneity on transversal coronal loop oscillations (2008, background): “In younger active region loops there have been measurements of “super-hydrostatic” scale heights that are up to four times higher than expected (Aschwanden et al. 2000, 2001).”
Dynamics of solar coronal loops I. Condensation in cool loops and its effect on transition region lines (2003, background): “…mechanisms of coronal heating have been proposed (e.g. wave heating, nanoflares, magnetic reconnection), but independent of the detailed process of energy release there is now observational evidence that coronal loops are predominantly heated at the footpoints (Aschwanden et al. 2000, 2001).”
MULTISPECTRAL EMISSION OF THE SUN DURING THE FIRST WHOLE SUN MONTH: MAGNETOHYDRODYNAMIC SIMULATIONS (2008, result): “It appears too low in EIT 171 Å: this seems to be in agreement with the results of Aschwanden et al. (2001), who found that steady-state models do not reproduce correctly loop emission but they only show bright end points, thus indicating that dynamic solutions may be necessary to improve the match…”
Physics of Solar Prominences: II—Magnetic Structure and Dynamics (2010, background): “…recent analysis of TRACE observations of some coronal loops independently indicated that the heating is concentrated near the loop footpoints (Aschwanden et al., 2001; Winebarger et al., 2002), the observational evidence for the spatial distribution of coronal heating is inconclusive at best.”
Coronal loop seismology using multiple transverse loop oscillation harmonics (2007, background): “This is not abnormal, as the stratification inside coronal loops may exceed the hydrostatical value by a factor of 4 (see Aschwanden et al. 2000, 2001).”
An Ab Initio Approach to the Solar Coronal Heating Problem (2004, methodology): “This balance is for a typical point in time, and it is obvious that the heating in the corona is decreasing with height, as found from TRACE data by a number of authors (Schrijver et al. 1999; Aschwanden et al. 2000a, 2001).”