"This is very unexpected, and challenges current numerical simulations, which suggest that stars like these should not be able to sustain differential rotation
of this magnitude," said Othman Benomar, research associate at the NYU Abu Dhabi Center for Space Science and lead author of the study published in Science Magazine.
The new model determined that solar seasons originate from the interaction of large-scale planetary waves known as Rossby waves and differential rotation
, which is the fact that the sun's equator rotates more rapidly than its poles.
This differential rotation
stretches out the field along the equator, (v is for velocity)
With this he studied the differential rotation
of Sun between 1901 and 1906 (see Halm, 1904) and was awarded the Brisbane medal of the Royal Society of Edinburgh.
of stars, magnetic and magnetorotational instabilities are discussed thoroughly and a theory of driven turbulence in formulated using both simulations and observations.
During bending, the plates may undergo differential rotation
due to the difference in the levels of the bottom surface of the slab and flange.
The outer layers of the Sun exhibit differential rotation
. At the equator, the surface rotates once every 25.4 days; near the poles, it's as much as 36 days.
This likelihood of frequent flips "makes it very attractive to monitor tau Bootis and possibly other similar stars with high differential rotation
, which may improve our understanding of the generation and dynamics of magnetic fields in stars," says Marina Romanova of Cornell University.
Its outer layers exhibit differential rotation
, at the equator the surface rotates once every 25.4 days but near the poles it's as much as 36 days.
Previous models of stellar convection were limited to small areas on the star's surface, too small to help researchers understand how differential rotation
Such globally coherent magnetic fields arise because our star's outer, convective layer of ionized gas slides across the lower, non-convective layer faster at the equator than it does at the poles, called differential rotation
. This process stirs up plasma and creates a cyclic field.
We have been studying through 3-D global simulations the nature of both differential rotation
and dynamo action that can be achieved in G-type stars like the sun by turbulent convection in their outer envelopes, and also by core convection in more massive A-type stars.