S. Wedemeyer, T. Bastian, R. Brajša, M. Barta, H. Hudson, G. Fleishman, M. Loukitcheva, B. Fleck, E. Kontar, B. De Pontieu, S. Tiwari, Y. Kato, R. Soler, P. Yagoubov, J. H. Black, P. Antolin, S. Gunar, N. Labrosse, A. O. Benz, A. Nindos, M. Steffen, E. Scullion, J. G. Doyle, T. Zaqarashvili, A. Hanslmeier, V. M. Nakariakov, P. Heinzel, T. Ayres, M. Karlickye, and the SSALMON Group

SSALMON - The Solar Simulations for the Atacama Large Millimeter Observatory Network

Figure 3. Detailed comparisons with ALMA observations (left) with numerical models (right) enable us to develop observing strategies for ALMA, to plan, optimize, and interpret observations, and to demonstrate that potentially important scientific results can be expected from solar ALMA observations.

Abstract

The Solar Simulations for the Atacama Large Millimeter Observatory Network (SSALMON) was initiated in 2014 in connection with two ALMA development studies. The Atacama Large Millimeter/submillimeter Array (ALMA) is a powerful new tool, which can also observe the Sun at high spatial, temporal, and spectral resolution. The international SSALMONetwork aims at co- ordinating the further development of solar observing modes for ALMA and at promoting scientific opportunities for solar physics with particular focus on numerical simulations, which can provide important constraints for the observing modes and can aid the interpretation of future observations. The radiation detected by ALMA originates mostly in the solar chromosphere – a complex and dynamic layer between the photosphere and corona, which plays an important role in the transport of energy and matter and the heating of the outer layers of the solar atmosphere. Potential targets include active regions, prominences, quiet Sun regions, flares. Here, we give a brief overview over the network and potential science cases for future solar observations with ALMA.

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Last Revised: 2015 March 2nd