Dear Colleagues.
We would like to invite you to submit contributed abstracts to the “The Solar Atmosphere and Heliosphere: Atomic Processes, Spectroscopy, and Diagnostics” session at the upcoming Asia Oceania Geosciences Society (AOGS) in Japan later this year. The full session description is given below. The 11th Annual AOGS meeting will take place in Sapporo, Japan, 28 July to 01 August 2014. The Conference WebPages can be found here: http://www.asiaoceania.org/aogs2014/ along with relevant link to the Mars Login for submitting abstracts as well as a link the list of Important Dates and links to other pertinent information.
The abstract-submission deadline is Tuesday 11 February 2014. The full abstract-submission details are given here: http://www.asiaoceania.org/aogs2014/public.asp?page=abstract.htm; but please note that the AOGS Conference Fee only covers two abstracts – any more than two abstracts to be presented by the same person would require additional fees.
Thank you in advance and we look forward to seeing you in Japan this coming summer!
Best regards,
Mario (on behalf of the ST28 Convenors).
Dr. Mario M. Bisi (RAL Space)
Dr. Helen E. Mason (University of Cambridge)
ST28: “The Solar Atmosphere and Heliosphere: Atomic Processes, Spectroscopy, and Diagnostics”
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.