Core Convection and Dynamos in Spectral Type O and B Stars

Details Core Convection and Dynamos in Spectral Type O and B Stars Core Convection and Dynamos in Spectral Type O and B Stars

May 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21642301a&link_type=abstract

American Astronomical Society, AAS Meeting #216, #423.01; Bulletin of the American Astronomical Society, Vol. 41, p.835

Astronomy and Astrophysics

Astronomy

Scientific paper

Recent observations have revealed that about one-third of O and B type stars have strong magnetic fields at their surfaces. It is currently unclear where these fields originate. In order to address this question, we examine the effects of core convection and magnetic dynamo processes within massive O and B stars with simulations in rotating spherical shells using the 3-D Spherical Harmonic (ASH) magnetohydrodynamic code.

Affiliated with

Also associated with

No associations

Rating

Core Convection and Dynamos in Spectral Type O and B 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 Core Convection and Dynamos in Spectral Type O and B Stars, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Core Convection and Dynamos in Spectral Type O and B Stars will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1891532