Transverse Oscillations in Coronal Loops Observed with TRACE – II. Measurements of Geometric and Physical Parameters

By Markus J. Aschwanden, B. de Pontieu, C. Schrijver, A. Title. 2002

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In Astronomy and Astrophysics

Citations in the corpus

Slow-mode standing waves observed by SUMER in hot coronal loops (2003, methodology): “1d, assuming a loop with a circular shape and using the same method as in Aschwanden et al. (2002).”
Hot coronal loop oscillations observed with SUMER: Examples and statistics (2003, methodology): “Distribution of the physical parameters of the 54 SUMER Doppler-shift oscillations (solid histograms), and distribution of the parameters of the 26 TRACE transversal loop oscillations (dotted histograms) obtained by Aschwanden et al. (2002).”
Observational Tests of Damping by Resonant Absorption in Coronal Loop Oscillations (2003, methodology): “We analyze 11 loop oscillation events from the study of Aschwanden et al. (2002) for which a reliable damping time tD has been determined (see, e.g., event 1 in Fig.”
Hinode observations of transverse waves with flows in coronal loops (2008, background): “The method requires high spatio-temporal resolution observations of the corona to resolve the wave motions that only became routinely available with the launch of SOHO spacecraft, and the Transition Region and Coronal Explorer (TRACE) satellite.”
Vertical oscillations of a coronal loop observed by TRACE (2004, methodology): “A number of transverse loop oscillations have been reported in a statistical study by Aschwanden et al. (2002), and most of them manifest clearly horizontal motions.”
Effect of longitudinal magnetic and density inhomogeneity on transversal coronal loop oscillations (2008, background): “These magnetoacoustic oscillations have been observed many times, e.g., Aschwanden et al. (1999a), Aschwanden et al. (2002), Nakariakov et al. (1999) and Verwichte et al. (2004) and have been identified as the standing fast kink mode from MHD wave theory developed by e.g., Edwin & Roberts (1983).”
Characteristics of transverse oscillations in a coronal loop arcade (2004, background): “The oscillation periods are in the range 200– 450 s, which is typical for transverse loop oscillations (Aschwanden et al., 2002).”
Damping of Coronal Loop Oscillations: Calculation of Resonantly Damped Kink Oscillations of One-dimensional Nonuniform Loops (2004, methodology): “As Goossens et al. (2002) did the exercise for a data set of 11 events obtained by Aschwanden et al. (2002), it became clear that the formula is pushed beyond its limit.”
Coronal loop oscillations Calculation of resonantly damped MHD quasi-mode kink oscillations of longitudinally stratified loops (2005, background): “Since then, several oscillating loops have been reported and thoroughly studied (Aschwanden et al. 2002; Schrijver et al. 2002; Nakariakov et al. 1999).”
MHD seismology of coronal loops using the period and damping of quasi-mode kink oscillations (2007, methodology): “We have repeated the procedure by considering uncertainties of 40% and 60% on the period and damping time respectively (Aschwanden et al. 2002).”
Standing Slow-Mode Waves in Hot Coronal Loops: Observations, Modeling, and Coronal Seismology (2010, methodology): “…with theoretical modeling have been used to estimate physical parameters of coronal plasma such as magnetic field (Nakariakov & Ofman 2001; Aschwanden et al. 2002; Wang et al. 2007), energy transport coefficients (Nakariakov et al. 1999; Ofman & Aschwanden 2002), density stratification…”
CORONAL LOOP OSCILLATIONS OBSERVED WITH ATMOSPHERIC IMAGING ASSEMBLY—KINK MODE WITH CROSS-SECTIONAL AND DENSITY OSCILLATIONS (2011, background): “This is in contrast to a statistical sample of 11 well-observed events with TRACE, where strong damping was found to be the rule, i.e., with τD/P ≈ 1.8 ± 0.8 (Aschwanden et al. 2002).”
The solar magnetic field (2006, background): “, [573, 574]) and slow mode type compressional oscillations at even longer frequencies [575] have been observed.”
Coronal loop oscillations - An interpretation in terms of resonant absorption of quasi-mode kink oscillations (2002, background): “Ofman & Aschwanden (2002) use the recent data base by Aschwanden et al. (2002) to investigate coronal loop oscillations in a sample of 11 loops.”
Multiwavelength Studies of MHD Waves in the Solar Chromosphere (2015, background): “…ranging from the deepest depths of the photosphere through to the outermost extremities of the corona (Ulrich 1970; Penn and Labonte 1993; Aschwanden et al. 1999, 2002, 2004; Nakariakov et al. 1999; Ballai et al. 2011; Morton et al. 2011; Scullion et al. 2011; Jess et al. 2012c;…”
Detection of Waves in the Solar Corona: Kink or Alfvén? (2008, methodology): “In an imaging instrument, the fast kink modes are observed as transversal displacements of coronal loops (Aschwanden et al. 2002).”