| Name: | Ambika Saxena |
| Affiliation: | Aryabhatta Research Institute of Observational Sciences |
| Conference ID : | ASI2024_628 |
| Title : | Exploring spectral line asymmetries due to the propagating MHD waves in the solar atmosphere |
| Authors : | Ambika Saxena1, Vaibhav Pant1 |
| Authors Affiliation: | Ambika Saxena, Vaibhav Pant (Aryabhatta Research Institute of Observational Sciences, Manora Peak, Nainital-263001, Uttarakhand, India) |
| Mode of Presentation: | Poster |
| Abstract Category : | Sun, Solar System, Exoplanets, and Astrobiology |
| 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 decades-long study of asymmetries in spectral lines observed from the solar corona and transition regions point toward mass and energy transport from the lower layers of the solar atmosphere to the corona. Two possible drivers for these asymmetries are found to be slow magnetoacoustic waves and jets (or plasma upflows). However, due to insufficient multi-wavelength observations and low spatial and spectral resolution of the current instruments, spectral line asymmetries due to transverse MagnetoHydro Dynamic (MHD) waves have not been observed yet. However, their study is possible by using 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 kink 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 showed the presence of spectral line asymmetries caused by these waves in an inhomogeneous plasma. We have also studied the statistical properties of these spectral line asymmetries and how they differ from the spectral line asymmetry caused by the plasma upflows. 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. |
