Speaker
Description
Decades-long studies of asymmetric spectral lines observed in the solar corona and the transition region point to mass and energy transport from the lower layers of the solar atmosphere to the corona. Slow magnetoacoustic waves and jets (plasma upflows) are considered to be the two possible drivers for these spectral line asymmetries. However, due to insufficient multiwavelength observations and the low spatial and spectral resolution of the current instruments, spectral line asymmetries due to the propagating transverse MHD waves have yet to be observed. We present evidence of the spectral line asymmetries caused by the transverse MHD waves propagating in the inhomogeneous plasma in the solar corona. We performed 3D MHD simulations and forward modeling for the Fe XIII (1074.9 nm) emission line. We also explored the possibility of observing these line asymmetries using modern ground-based facilities such as DKIST.
| Sessions | Novel diagnostic techniques and forward modelling |
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