|COOKIES: By using this website you agree that we can place Google Analytics Cookies on your device for performance monitoring.|
Heating and cooling of multistranded solar coronal loops
If you have a question about this talk, please contact Jérôme Guilet.
One big puzzle in Solar Physics is why coronal loops tracing the magnetic field lines are observed in EUV emission? In other words, what is the thermodynamic evolution of coronal loops? To tackle this issue, we use a 1D hydrodynamic model describing a loop as an amalgamation of strands evolving independently. The energy input is prescribed by the Parker model of nanoflare heating: discrete distribution of short bursts releasing energy (about 10^24 erg) along the loop. We first show that the model can reproduce the main observed features, especially focusing on the ubiquitous existence of blue-shifts in spectral observations. The modelled Doppler-shifts are a consequence of condensation at the foot-points of the loop inducing cool plasma moving downwards, and of evaporation generating outflows of hot material. The second step is to study the cooling of a previously heated loop, and to answer the following questions: what is the characteristic time-scale of cooling? what are the signatures of cooling in different pass-bands?
This talk is part of the Informal Lunch Seminars in AFD series.
This talk is included in these lists:
Note that ex-directory lists are not shown.
Other listsNumber Theory Study Group: Langlands correspondence Tools and Techniques for Speech Research Mini Courses in Theoretical Computer Science
Other talks"Ni-catalyzed Functionalization of Carbon Dioxide and C-O Bonds" Evolution of Mobile Network Infrastructure TBC - Emotion Sense & the use of mobile phone data Cavendish Graduate Student Conference on Physics 2014 Genomic technologies Fossil pollen and algae reveal Antarctica’s climate as the dinosaurs died out 66 million years ago