ALMA is providing many new opportunities for solar physics. The expert teams presented here focus on selected topics with A-F being more technical while G-P address particular scientific topics.
As of November 2015,the teams G-L and P have each composed a strategic document, which outlines prioritized science cases, anticipated outcome, technical requirements and (if applicable) observation strategies for the Cycle 4 and the CSV campaign in 12/2015. The documents have been combined into a white paper and may also serve as a basis for Cycle 4 observing proposals.
The secondary goal is to get an overview of necessary preparations for future observation campaigns (Cycle 5 and beyond) and the post-processing and analysis of ALMA data.
The exchange of useful information and cross-team collaborations are organized through activities that involve the whole SSALMONetwork, incl. regular team reports and workshops.
|A||Numerical models of the solar atmosphere|
|B||Radiative transfer and brightness temperature synthesis|
|C||Simulating instrumental effects for ALMA (incl. interferometric imaging)|
|D||Spectral lines in the millimeter range as new diagnostic tools|
|E||Emission mechanisms at millimeter wavelengths|
|F||Magnetic field measurements|
|G||Oscillations and waves|
|J||Chromospheric and coronal heating|
|K||Quiet Sun regions|
|L||Active regions and sunspots|
|M||Magnetic loops in the upper atmosphere|
|N||Space weather (inactive)|
|O||Implications for stellar physics - The solar-stellar connection|
|Q||ALMA Data Processing|