Meridian Circulation in Differentially Rotating Stars

Details Meridian Circulation in Differentially Rotating Stars Meridian Circulation in Differentially Rotating Stars

Dec 1972

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1972ap%26ss..19..309m&link_type=abstract

Astrophysics and Space Science, Volume 19, Issue 2, pp.309-349

Astronomy and Astrophysics

Astrophysics

9

Scientific paper

We formulate the first order theory of meridian circulation in radiative zones of approximate chemical homogeneity so as to allow calculation of circulation velocities in a star subject to an arbitrary axially symmetric angular velocity ω(r, θ). The calculation includes circulation due to perturbations in the nuclear burning rate. The formalism agrees with previous calculations relevant to special cases, and assumes maximum simplicity for rotation on cylinders. We find two types of steady state configurations: (1) rotation according to a special class of distributions ω(r, θ) which drive no currents, and (2) rotation according to arbitrary ω(r, θ), but with a correction to the molecular weight μ such that the net circulation velocity is zero. We find that a small μ gradient can quench the circulation in many cases. In particular, we conclude that a large differential rotation in the Sun might have escaped disruption by meridian currents, for a μ stratification of a few parts in 103.

Affiliated with

Also associated with

No associations

Rating

Meridian Circulation in Differentially 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 Meridian Circulation in Differentially Rotating Stars, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Meridian Circulation in Differentially Rotating Stars will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1640119