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SUMMARY:Numerical simulations of Red Giant Stars
DTSTART:20251203T130000Z
DTEND:20251203T140000Z
DTSTAMP:20260315T043000Z
UID:indico-event-9478@indico.fysik.su.se
DESCRIPTION:Speakers: Carolina Ortiz Rodriguez (Nordita/Univ. of Hamburg)\
 n\nWhen low-mass stars leave the main sequence\, their convective envelope
 s expand drastically\, leading to complex interactions between convection\
 , rotation\, and magnetic fields. Observations show a wide range of rotati
 on rates and magnetic activity behaviours\, yet the connection between rot
 ation profiles and angular momentum transport inside these stars remains p
 oorly understood.\nIn this work\, we study a 1 solar mass red giant star w
 ith a convection zone that reaches 80% of the star's radius. We use 3D hyd
 rodynamic and magneto-hydrodynamic star-in-a-box simulations at different 
 rotation rates. We analyse the flow structure\, differential rotation prof
 iles\, and we are currently computing the angular momentum flux contributi
 on to understand how rotation influences the transport processes inside th
 e star\, and how they shape the differential rotation profiles.\nPrelimina
 ry results show clear effects of rotation on the flow pattern and differen
 tial rotation amplitude\, with potential implications for the transport of
  angular momentum. Future work will include comparison with mean-field mod
 els.\n\nhttps://indico.fysik.su.se/event/9478/
LOCATION:Albano 3: 6335 - Hekto (10 seats) (Albano Building 3)
URL:https://indico.fysik.su.se/event/9478/
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