Three‐dimensional numerical simulation of MHD waves observed by the Extreme Ultraviolet Imaging Telescope

By S. Wu, Huinan Zheng, S. Wang, Barbara J. Thompson, S. Plunkett, Xuepu Zhao, M. Dryer. 2001

166 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/5b4c487db4bf7bacc3a2424dc3527afbf45b6d32

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In Astronomy and Astrophysics

Citations in the corpus

On the nature of EIT waves, EUV dimmings and their link to CMEs (2004, methodology): “It should be stressed, however, that to account for the low EIT wave velocities both models (Wang 2000; Wu et al. 2001) had to adopt values of the coronal magnetic field resulting in high values of the plasma parameter beta (β > 1).”
The Kinematics of a Globally Propagating Disturbance in the Solar Corona (2008, methodology): “This interpretation has been used to create numerical simulations which closely imitate the observed data (Wu et al. 2001; Ofman & Thompson 2002; Ofman 2007).”
A multiwavelength study of solar flare waves II. Perturbation characteristics and physical interpretation (2004, methodology): “Following the simulated wavefronts in Uchida et al. (1973) and Wu et al. (2001), the shock front is tilted towards the solar surface; this is caused by the increase of vA with height in the low corona at larger distances from an AR (Mann et al. 1999).”
Solar Phenomena Associated with “EIT Waves” (2002, methodology): “Moreton waves have been modeled by Uchida (1968, 1974) as a fast-mode MHD wave, and additional modeling has shown this description may work equally well or better for EIT waves (Wang 2000; Wu et al. 2001).”
Solar winds driven by nonlinear low‐frequency Alfvén waves from the photosphere: Parametric study for fast/slow winds and disappearance of solar winds (2005, methodology): “The method is similar to that in the work of Wu et al. [2001] , while ours is implemented for stable treatment of strong MHD shocks.”
OBSERVATIONS AND INTERPRETATION OF A LOW CORONAL SHOCK WAVE OBSERVED IN THE EUV BY THE SDO/AIA (2011, background): “…of the more common diffuse EUV waves is still being debated as to whether they are fastmode MHD waves (e.g., Wills-Davey & Thompson 1999; Wang 2000; Wu et al. 2001; Ofman & Thompson 2002; Schmidt & Ofman 2010), slow-mode MHD waves (Wang et al. 2009), or non-waves related to a current shell or…”
NUMERICAL SIMULATION OF AN EUV CORONAL WAVE BASED ON THE 2009 FEBRUARY 13 CME EVENT OBSERVED BY STEREO (2009, background): “…only the expanding flux tube, neglecting interaction with the surroundings (Delannée et al. 2008), simulated the interaction of coronal waves with only a local active region (Uchida 1974; Ofman & Thompson 2002), or they drove the coronal wave by a pressure pulse (Wang 2000; Wu et al. 2001).”
EUV WAVE REFLECTION FROM A CORONAL HOLE (2009, methodology): “This is confirmed by numerical simulations (Wang, 2000; Wu et al. 2001).”
Advances in Observing Various Coronal EUV Waves in the SDO Era and Their Seismological Applications (Invited Review) (2014, unknown): “For example, Wu et al. (2001) found that a fast-mode wave in a coronal region of β ≈ 1 can explain an observed EIT wave.”