| Name: | Ambika Saxena |
| Affiliation: | Aryabhatta Research Institute of Observational Sciences |
| Conference ID : | ASI2023_316 |
| Title : | Exploring spectral line asymmetries due to the propagating MHD waves in the solar atmosphere |
| Authors : | Ambika Saxena , JRF , ARIES, Nainital
Dr. Vaibhav Pant, Scientist-C, ARIES, Nainital |
| Mode of Presentation: | Poster |
| Abstract Category : | Sun and the Solar System |
| Abstract : | MHD waves are considered to be one of the candidates for coronal heating and solar wind acceleration, so, understanding their spectroscopic properties and propagation through different layers of the solar atmosphere is important. Over a decade-long study of asymmetries in spectral lines observed from solar coronal and transition region point towards mass and energy transport from lower layers of the solar atmosphere to the corona. Two possible drivers for these asymmetries are slow magnetoacoustic waves and jets and upflows. However, due to insufficient multi-wavelength observations and low spatial and spectral resolution of the current instruments, spectral line asymmetries due to fast transverse MagnetoHydro Dynamic (MHD) waves have not been observed yet. But their study is possible by MHD simulations. In this study, we used the forward-modelled data for the Fe XIII emission line obtained from 3D MHD simulations using MPI-AMRVAC for propagating fast transverse waves. The ‘Modified Blue-Red (BR) Asymmetry’ technique was applied to this data to obtain BR asymmetry profiles. Our analysis for the simulation of a coronal hole region driven by propagating fast transverse MHD waves showed the presence of spectral line asymmetries caused by these waves in an inhomogeneous plasma. These asymmetries are expected to be observed by future ground and space-based facilities such as Visible Emission Line Coronagraph (VELC) onboard Aditya-L1 and DKIST. We also plan to study the spectral line asymmetries for the data integrated for different lines of sight and other associated properties.
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