Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003agufmsh42b0536b&link_type=abstract
American Geophysical Union, Fall Meeting 2003, abstract #SH42B-0536
Astronomy and Astrophysics
Astrophysics
7500 Solar Physics, Astrophysics, And Astronomy, 7524 Magnetic Fields, 7539 Stellar Astronomy, 7544 Stellar Interiors And Dynamo Theory
Scientific paper
Observationally, it has been found that magnetic activity is a strong function of rotation rate. The connection between rotation and dynamo-generated fields is not well understood, however. The typical interface dynamo theory applied to the Sun to describe its activity cycle assumes the existence of a velocity shear layer. Such a model is inappropriate for fully convective stars that are nevertheless active, such as late-type M and L stars and pre-main sequence T Tauri stars; in these stars a turbulent dynamo is generally believed to be the mechanism of magnetic field generation. We investigate the connection between observed activity behavior and magnetic field generation in fully convective stars through a series of simulations of the turbulent dynamo. The simulations were performed in a Cartesian domain using ANMHD, a 3D MHD anelastic code. We compare the resulting magnetic topologies for a series of Rossby numbers and comment on the implications for the sizes of coronal loops and activity levels.
Abbett William P.
Bercik David John
Fan Ying
Fisher George H.
No associations
LandOfFree
Turbulent Magnetic Field Generation in Rotating Stars does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Turbulent Magnetic Field Generation in Rotating Stars, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Turbulent Magnetic Field Generation in Rotating Stars will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1647450