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SUMMARY:Power supply and evolution of the solar dynamo
DTSTART;VALUE=DATE-TIME:20230511T093500Z
DTEND;VALUE=DATE-TIME:20230511T095000Z
DTSTAMP;VALUE=DATE-TIME:20240704T115652Z
UID:indico-contribution-338@meetings.aip.de
DESCRIPTION:Speakers: Quentin Noraz (Rosseland Centre for Solar Physics\, 
 University of Oslo\, P.O. Box 1029 Blindern\, Oslo\, NO-0315\, Norway)\nTh
 e solar magnetic field is generated and sustained by the combined action o
 f turbulent convection and differential rotation. This dynamo process can 
 sometimes lead to magnetic cyclic variabilities\, like the solar 11 years 
 cycle. Traces of magnetic cycles have also been detected in other solar-li
 ke stars\, ranging from a few years to a few tens of years. How is the sol
 ar cycle period controlled?\nRecent 3D numerical simulations of solar-like
  stars show that different regimes of differential rotation can be charact
 erized with the Rossby number (advection over Coriolis force). In particul
 ar\, “anti-solar” differential rotation (fast poles\, slow equator) ma
 y appear for high Rossby number (slow rotators). If large-scale flows tran
 sitions occur during the solar main sequence\, we may wonder how the magne
 tic generation will be impacted.\n\nWe present a numerical multi-D study t
 o understand the magnetic field generation and evolution of solar-like sta
 rs under various differential rotation regimes\, in a Sun in time context.
  We find that short and local cycles near the surface are favoured for sma
 ll Rossby numbers (fast rotators)\, while long and global cycles appear fo
 r intermediate (solar-like) Rossby numbers. Slow rotators (high Rossby num
 ber) are found to produce statistically steady dynamo with no cyclic activ
 ity in most cases considered. We further evaluate energy transfers in thes
 e models and quantify that dynamos can be powered by up to 3% of the stell
 ar luminosity\, part of it being then available to power surface events. I
 n this regard\, future Solar Orbiter observations outside the ecliptic wil
 l provide fantastic constraints on solar polar caps magnetic field\, and t
 hus on the type of dynamo that our Sun is most likely to operate.\n\nhttps
 ://meetings.aip.de/event/24/contributions/338/
LOCATION:Haus H\, Telegrafenberg
URL:https://meetings.aip.de/event/24/contributions/338/
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