The detection of 3 & 5 min period oscillations in coronal loops

By I. Moortel, J. Ireland, A. Hood, R. Walsh. 2002

182 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/45ec869f31ade623d5df2eaa97161dedaffe6a55

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In Astronomy and Astrophysics

1. Tongjiang Wang
2. S. Solanki
3. R. Erdélyi
4. L. Ofman
5. E. Khomenko
6. G. D. Zanna
7. Manel Collados
8. D. Innes

In Molecular Biology

1. Tongjiang Wang
2. R. Erdélyi
3. L. Ofman
4. Manel Collados
5. E. Khomenko
6. G. Verth
7. I. Moortel
8. S. Solanki

Citations in the corpus

• How to Channel Photospheric Oscillations into the Corona (2005, methodology): “…well the simulations reproduce the observed properties of the propagating waves, we calculate coronal intensities from the model (∼n ), rebin to the spatial (2 ) and2e temporal (30 s) resolution of theTRACE data considered by De Moortel et al. (2002b), and calculate the (90 s) running difference.”
• Magnetic field inclination and atmospheric oscillations above solar active regions (2006, background): “However, at least above the (ramp reduced) acoustic cut-off frequency, energy may also propagate upwards into the overlying atmosphere (e.g. Brynildsen et al. 2002; De Moortel et al. 2002), with observationally testable consequences.”
• Hot Coronal Loop Oscillations Observed by SUMER: Slow Magnetosonic Wave Damping by Thermal Conduction (2002, methodology): “The damping by thermal conduction of the slow waves in TRACE loops was considered by De Moortel et al. (2002a).”
• Oscillations and Waves in Sunspots (2015, methodology): “Similarly, De Moortel et al. (2002) detected intensity oscillations with TRACE 171 Å Living Reviews in Solar Physics DOI 10.1007/lrsp-2015-6 20 Elena Khomenko and Manuel Collados data at the footpoints of coronal loops situated above sunspot regions.”
• Multiwavelength Studies of MHD Waves in the Solar Chromosphere (2015, background): “De Moortel et al. (2002) suggested that the most likely explanation would be a photospheric driver directly exciting the magnetic footpoints of the fan and plume structures.”
• Hot coronal loop oscillations observed with SUMER: Examples and statistics (2003, background): “…offprint requests to: T.J. Wang nal loops by the EUV Imaging Telescope (EIT) (Berghmans & Clette 1999), later confirmed by TRACE observations (De Moortel et al. 2000; 2002a;b;c; Robbrecht et al. 2001), and identified as propagating slow waves (Nakariakov et al. 2000; Tsiklauri & Nakariakov…”
• Solar active regions: SOHO/CDS and TRACE observations of quiescent coronal loops (2003, background): “Both plumes and these types of loops have simple geometries, are anchored in regions of high magnetic flux concentrations, and have periodical variations in intensities, interpreted as slow magnetoacustic waves (see, e.g., De Moortel et al. 2002, and references therein).”