| Session Description |
This session will cover general contributions on any aspect of Heliophysics concerning the Sun and Heliosphere that are not suited to other sessions in addition to specialist contributions on the atomic physics of the solar atmosphere and heliosphere. The solar atmosphere holds the key to some of the most-fundamental and open questions remaining in Heliophysics. The need for accurate atomic data has always been essential for the realistic modelling of astrophysical plasmas and hence our understanding of the Sun. One of the key questions in Heliophysics pertains to precisely how the corona is heated (the coronal heating problem). Others questions include (but are not limited to): how the solar wind is accelerated; how much short-wavelength radiation does the Sun irradiate and exactly how does this affect the Earth’s atmosphere; and what links, if any, does short-wavelength solar irradiance have on the Earth’s long-term climate? This session is intended to cover key aspects of atomic physics related to the solar plasma, from the solar interior, through the photosphere, chromosphere, transition region and corona, all the way to the edge of the heliosphere. Contributions are solicited from those developing models/simulations (Bifrost, NRLSSI, etc…), from atomic database providers (ADAS, CHIANTI, etc…) and from those analysing the most-recent solar observations (IRIS, SOHO, SDO, Hinode, etc…), or indeed any other relevant contributions, for example concerning the importance of non-equilibrium processes. The understanding of solar atomic physics also plays an important part in our comprehension and prediction of space weather effects at Earth and on our understanding of the Earth’s long-term climate variation. |
