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SUMMARY:Magnetism of solar-like and intermediate-mass stars: numerical exp
 eriments - Dr. Laurene Jouve (IRAP\, Toulouse)
DTSTART:20140428T150000Z
DTEND:20140428T160000Z
UID:TALK50937@talks.cam.ac.uk
CONTACT:Adrian Barker
DESCRIPTION:In this talk\, we will review some aspects of the stellar magn
 etism and in particular what numerical simulations tell us about the physi
 cal processes underlying the observations.\n\nIn solar-like stars\, a conv
 ective dynamo is thought to be responsible for the presence and evolution 
 of magnetic fields. One step of this dynamo process is the emergence of ma
 gnetic flux from the interior where it is created and organised to the ext
 erior where it emerges as sunspots. We will show the results of 3D numeric
 al simulations of such a process.\n\nIntermediate-mass stars have a probab
 ly different type of magnetism. Some A stars (Ap stars) possess strong lar
 ge-scale magnetic fields which seem to remain rather stable in time. Some 
 recent observations now tend to show that another class of A stars exists\
 , which exhibit a more complex and weak magnetic field\, organized at smal
 ler scales at their surfaces. We try to understand such a magnetic dichoto
 my by numerically investigating the stability of magnetic fields created b
 y differential rotation in the stellar radiative envelope.
LOCATION:MR14\,  Centre for Mathematical Sciences\, Wilberforce Road\, Cam
 bridge
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