Abstract Details
| Name: Megha A Affiliation: Indian Institute of Astrophysics Conference ID: ASI2016_486 Title : Coronal Plasma Diagnostics using Visible and Near-IR Coronal Emission Lines Authors and Co-Authors : A. Megha(2), K. Sankarasubramanian(1, 2), , Jagdev Singh(2), M. Sampoorna(2), and K. N. Nagendra(2) (1) Space Astronomy Group, ISRO Satellite Centre, Bengaluru (2) Indian Institute of Astrophysics, Koramangala, Bengaluru Abstract Type : Poster Abstract Category : Sun and the Solar System Abstract : Solar Corona consists of high temperature dynamics plasma (of the order of Million degree). The physical parameters of the coronal plasma (viz. Temperature, densities, magnetic field etc.) are dynamic. Though it is well known that the average temperature of the plasma is about Million degree, it changes drastically during eruptive events like flares and CMEs. Even during quiet period, the volume of plasma is considered to be multi-thermal (i.e., more than one temperature inside the volume). Simultaneous spectroscopy of multi spectral line is the best diagnostic method in order to study such a dynamic plasma. The physical parameters of the plasma are derived using line ratio methods. In this work, we incorporate a forward modeling technique for the observed data using the CHIANTI databases and its spectral synthesis capabilities. The motivation behind this work is to study the feasibility of generating an inversion procedure for spectral lines formed in solar coronal plasma like it is carried out for the photospheric and chrmospheric spectral lines. This study includes the derivation of the major plasma parameters - Temperature, densities and Emission Measures. This study would also discuss the forward modeling for coronal magnetic field observations and hence help with the data from the upcoming Aditya mission. The sailent advantages and disadvantages of this methodology would also be brought out in this study. |