Standing Slow-Mode Waves in Hot Coronal Loops: Observations, Modeling, and Coronal Seismology
By Tongjiang Wang. 2010
148 citations recorded by the source corpus.
Strongly damped Doppler shift oscillations are observed frequently associated with flarelike events in hot coronal loops. In this paper, a review of the observed properties and the theoretical modeling is presented. Statistical measurements of physical parameters (period, decay time, and amplitude) have been obtained based on a large number of events observed by SOHO/SUMER and Yohkoh/BCS. Several pieces of evidence are found to support their interpretation in terms of the fundamental standing longitudinal slow mode. The high excitation rate of these oscillations in small- or micro-flares suggest that the slow mode waves are a natural response of the coronal plasma to impulsive heating in closed magnetic structure. The strong damping and the rapid excitation of the observed waves are two major aspects of the waves that are poorly understood, and are the main subject of theoretical modelling. The slow waves are found mainly damped by thermal conduction and viscosity in hot coronal loops. The mode coupling seems to play an important role in rapid excitation of the standing slow mode. Several seismology applications such as determination of the magnetic field, temperature, and density in coronal loops are demonstrated. Further, some open issues are discussed.
Subfields: Astronomy and Astrophysics, Molecular Biology
View Paper: https://www.semanticscholar.org/paper/910c464d439e9d250d27156d6dcb45ec8400987e
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In Astronomy and Astrophysics
- T. Van Doorsselaere
- Valery M. Nakariakov
- G. Verth
- Tongjiang Wang
- Giuseppe Nisticò
- R. Erdélyi
- Iñigo Arregui
- L. Ofman
In Molecular Biology
- G. Verth
- Valery M. Nakariakov
- T. Van Doorsselaere
- Giuseppe Nisticò
- L. Ofman
- Iñigo Arregui
- R. Erdélyi
- E. Kupriyanova
Citations in the corpus
- Coronal Heating by MHD Waves (2020, background): “7, excluding the regions of the thermal mode instability, could be responsible for the observed rapid damping of slow waves in the corona (Wang 2011).”
- Magnetohydrodynamic Oscillations in the Solar Corona and Earth’s Magnetosphere: Towards Consolidated Understanding (2016, background): “Typical periods range in 7–31 min; typical decay times are usually one or two oscillation periods; and typical amplitudes are 50–100 km s−1 that makes the relative amplitude up to 30 % of the sound speed (see Wang 2011, for a comprehensive review).”
- Multiwavelength Studies of MHD Waves in the Solar Chromosphere (2015, background): “Such detailed overviews include quasi-periodic (Nakariakov et al. 2005), standing (Wang 2011), magnetoacoustic (Van Doorsselaere et al. 2009b; De Moortel 2009) and Alfvén (Mathioudakis et al. 2013) waves.”
- Quasi-periodic Pulsations in Solar and Stellar Flares: An Overview of Recent Results (Invited Review) (2016, background): “Moreover, such a mechanism may be responsible for the standing slow waves observed in hot flare loops with SUMER (Wang, 2011; Yuan et al., 2015).”