We had the first meeting in Bern the week of the 29th April 2024, monday to friday. We focused on many different topics.
Resonant excitation
Atomic models
Line Forward Modelling
Global MHD
Multiwavelength, multi-mission
Listing the approximations and functionalities of the different codes.
To make progress in our understanding of the underlying emission mechanisms at play in the Middle Corona, we have coordinated a study comparing key observations and forward models. We compared methods and codes for the calculation of line intensities affected by resonant excitation, from the EUV to the NIR, and are currently testing for the minimum necessary atomic models and associated uncertainties. The models and codes benchmarked were: FORWARD (Gibson et al., 2016), GHOSTS (Gilly & Cranmer, 2020), Gilly & Cranmer, 2020, MAS (Mikić and Linker (1996), Mikić et al. (1999), Linker et al. (1999), Lionello et al. (2008), Downs et al. (2013) , Mikić et al. (2018)), P-CORONA (see Supriya et al. 2021), and three custom codes that have been produced by F. Auchère, G Del Zanna, and S. Giordano. We tryed first spherically symmetric (quiet sun vs coronal hole) on the hydrogen and coronal iron lines.
Benchmark against 2024 eclipse – A proposal for an ISSI workshop was submitted, led by Jenna Samra.
Look forward to the next eclipse and make recommendations for what to do.
The models below show the predicted Lyman Alpha emission in photons cm^-2 s^-1 sr^-1, along a streamer (Gibson et al 1999) as a function of height for the various benchmarked models. The corresponding Log plot show’s the profiles as a function of distance on a logarithmic axes.
