New insights about the past, present and future of solar magnetism | Quentin Noraz
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19.01.2023
Co-author
Affiliation
Rosseland Centre for Solar Physics, University of Oslo, Norway
Main category
Natural Sciences (Astrophysics and Astrononmy)
Caption
The magnetic field of solar-type stars is generated and sustained through an internal dynamo process. This process is mostly determined by the combined action of turbulent convective motions and differential rotation. It can sometimes lead to magnetic cyclic variabilities, like the 11-years solar cycle. Evidence of magnetic cycles have been detected for other solar-type stars as well, ranging from a few years to a few tens of years. How are these cycles controlled? Observations and stellar evolution models show that solar-like stars spin-down during their main-sequence. In parallel, numerical simulations of these stars show that different regimes of differential rotation can be reach and are characterized with the Rossby number. Read more at https://espos.stream/2022/12/01/Noraz/.
Further information
Further reading
Link to the European Solar Physics Online Seminars (ESPOS) webpage: https://espos.stream/2022/12/01/Noraz/
Language
English
DOI
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