How is the Sun’s outer atmosphere so darn hot?
Oscillations, in the form of slow/fast magneto-acoustic and Alfvén waves, are often presented as a principal component in transferring vast quantities of energy flux into the solar chromosphere and corona.
Research on the wave activity is highly dominated by those in the corona. As a result, there is less focus on the complexities associated with interpreting MHD wave phenomena in the solar photosphere and chromosphere.
The WaLSA Team focuses on challenges faced in wave studies in the lower solar atmosphere.
A chromospheric resonance cavity in a sunspot mapped with seismologyNature Astronomy, 2020, 4, 220
Resonance cavity (the pink isocontours) observations above a sunspot, amplifying propagating magentic waves in the lower solar atmosphere.
Transverse oscillations in slender Ca II H fibrils observed with Sunrise/SuFIAstrophysical Journal Supl. Ser., 2017, 229, 9
Transverse-wave propagations in slender bright fibrils near a small solar active region, carrying a vast amount of energy in to the low solar chromosphere.
Photospheric observations of surface and body modes in solar magnetic poresAstrophysical Journal, 2018, 857, 28
Direct evidence of surface and body wave modes in numerous pores, implying how these modes transfer energy from the waveguide to the surrounding plasm.
The WaLSA Team interactively engages with the public about its activitiy and science. This hopefully creates opportunities for learning, developing new skills, gaining new insights or ideas, developing better research, raising aspiration, or being inspired.