Evidence for Nonuniform Heating of Coronal Loops Inferred from Multithread Modeling of TRACE Data

By Markus J. Aschwanden, R. Nightingale, D. M. Alexander. 2000

251 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/f130c9560e4443cbc4d0588295a35bfdefb0027e

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Citations in the corpus

Hinode observations of transverse waves with flows in coronal loops (2008, methodology): “The thin-threaded coronal loop structure is consistent with past models of coronal loops (e.g., Aschwanden et al. 2000; Ofman & Aschwanden 2002).”
Coronal Loops: Observations and Modeling of Confined Plasma (2010, methodology): “Attempts of systematic studies have been performed in the past on Yohkoh and TRACE data (e.g., Porter and Klimchuk, 1995; Aschwanden et al., 2000).”
RHESSI Microflare Statistics. I. Flare-Finding and Frequency Distributions (2008, background): “In the ‘‘quiet’’ Sun, outside of active regions, Yohkoh SXT, the Transition Region and Coronal Explorer (TRACE ), and the SOHO Extreme Ultraviolet Imaging Telescope (EIT) have detected ‘‘nanoflares’’ down to 1025 erg (Krucker et al. 1997; Krucker & Benz 1998; Aschwanden et al. 2000; Benz & Krucker 2”
Elementary Loop Structures in the Solar Corona Analyzed from TRACE Triple-Filter Images (2005, methodology): “…0:56) ; 109 cm 3 for 30 loops detected in 171 8 with EIT (Aschwanden et al. 1999), ne ¼ (2:44 0:87) ; 109 cm 3 for 18 loops detected in 195 8 with EIT (Aschwanden et al. 2000a), ne ¼ (3:12 1:00) ; 109 cm 3 for 17 loops detected in 284 8 with EIT (Aschwanden et al. 2000a), and ne 109 cm 3 for 41…”
Slow magnetoacoustic waves in coronal loops: EIT and TRACE (2001, background): “For a more elaborate calculation of noise see Berghmans & Clette (1999) for EIT and Aschwanden et al. (2000a) for TRACE.”
Hot coronal loop oscillations observed with SUMER: Examples and statistics (2003, background): “…width along the slit in an oscillatory region may be due to the fine structure of a coronal loop which may consist of a large number of fine threads as seen in TRACE 171 and 195 Å images (Aschwanden et al. 2000); different threads can have different densities and possibly different temperatures.”
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).”
An Ab Initio Approach to the Solar Coronal Heating Problem (2004, background): “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).”
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).”
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).”
Transverse Oscillations of Coronal Loops (2009, background): “Moreover, it has been suggested by, e.g., Aschwanden et al. (2000) that the loops as we see them actually consist of a multitude of individual loop strands.”
Coronal loop seismology using multiple transverse loop oscillation harmonics (2007, background): “This fact, however, is compatible with the findings of Aschwanden et al. (2000).”
Nanoflare Statistics from First Principles: Fractal Geometry and Temperature Synthesis (2002, methodology): “…with single instruments in a restricted temperature range (e.g., Berghmans, Clette, & Moses 1998; Krucker & Benz 1998; Parnell & Jupp 2000; Aschwanden et al. 2000b, 2000c), while only few studies with more comprehensive temperature coverage exist (Berghmans, McKenzie, & Clette 2001;…”
Solar active regions: SOHO/CDS and TRACE observations of quiescent coronal loops (2003, methodology): “Aschwanden et al. (2000) analysed a large number of TRACE loops, deriving density and temperature profiles.”