Dear Colleagues.
I would like to draw your attention to the ST33 session: ‘Multi-scale plasma wave processes in the solar atmosphere’ in the framework of Asia Oceania Geosciences Society (AOGS) meeting.
The 12th Annual AOGS will take place in Singapore, 2-7 August 2015. Further details regarding abstract submission, registration, accommodation and relevant deadlines can be found on the meeting website:
http://www.asiaoceania.org/aogs2015/public.asp?page=home.htm
Important! Abstract submission deadline is 18 February 2015.
ST33: ‘Multi-scale plasma wave processes in the solar atmosphere’
Conveners:
Viktor Fedun (The University of Sheffield, UK), v.fedun@sheffield.ac.uk
Leon Ofman (Catholic University of America and NASA Goddard Space Flight Center, United States), Leon.Ofman@nasa.gov
Dipankar Banerjee (Indain Institute of Astrophysics, India), dipu@iiap.res.in
Session Description
Multi-scale plasma wave processes play a fundamental role for energy transfer from the lower solar atmosphere to corona. The innovative “new generation” hi-resolution solar observing instruments (IBIS/DST, CRISP/SST, ROSA/DST, IRIS, Hinode, SDO, Hi-C) have provided a step-change in understanding the non-thermodynamic physical mechanisms contributing to solar atmospheric heating. Concurrently, results of cutting-edge numerical simulations, hi-resolution observations and theoretical development have produced great advances in multi-scale plasma modelling and data inversion. Scientific debate is still on-going as to how observed MHD-scale waves generated at the photospheric region can be transformed into much smaller (kinetic) length scales where heating processes become more efficient. The current numerical modelling of solar atmospheric waves is separated by two main physical regimes i.e. MHD and kinetic. The large-scale MHD simulations of the wave processes in the lower solar atmosphere include the effects of radiation and partial ionisation. The question is: do contemporary MHD simulations have anything like time/space resolution and the complex magnetic topology (and the additional observed properties such as flux emergence, cancellation, shearing, granular buffeting) required to adequately model what is happening in the small-scale wave/reconnection/heating events? This is the key motivation of the proposed session.
With our Best Regards,
Viktor Fedun, Leon Ofman and Dipankar Banerjee