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SUMMARY; CHARSET=UTF-8 :Convection-driven differential rotation in stars and giant planets (Dr Loren Matilsky)
UID:exeter_event_14223
URL:http://www.exeter.ac.uk/events/details/?event=14223
DTSTART;VALUE=DATE:20240918T143000
DTEND;VALUE=DATE:20240918T153000
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ORGANIZER: MAILTO:s.i.thomson@exeter.ac.uk
ATTACH: http://www.exeter.ac.uk/events/details/?event=14223
DTSTAMP:20240912T111230
LOCATION:Harrison Building 106 
DESCRIPTION; CHARSET=UTF-8 :Abstract: Most (if not all) rotating spherical fluid bodies that we can observe exhibit some sort of differential rotation. Namely, when the rotation rate is averaged in longitude and/or time, this rate varies with latitude. On the Sun, the differential rotation is monotonic; the equator rotates roughly 30% faster than the polar regions. On Jupiter, on the other hand, the rotation rate exhibits many alternating fast and slow bands, or jets. Both types of differential rotation should, in theory, be understandable in terms of convection and its overshoot into adjacent layers of stable stratification (and magnetism of course, especially in the Sun). In this talk I will summarise our current understanding of how convection drives differential rotation in each type of system (say, "solar" and "Jovian"). I will also describe several global simulations of convection and magnetism, which were designed to address some unique processes that affect differential rotation (1) The joint presence of http://www.exeter.ac.uk/events/details/?event=14223
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