Hydrogen Abundance in the Tachocline Layer of the Sun

Details Hydrogen Abundance in the Tachocline Layer of the Sun Hydrogen Abundance in the Tachocline Layer of the Sun

Oct 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003pasj...55.1015t&link_type=abstract

Publications of the Astronomical Society of Japan, Vol.55, No.5, pp. 1015-1023

Astronomy and Astrophysics

Astronomy

2

Sun: Abundances, Sun: Helioseismology, Sun: Interior, Sun: Oscillations

Scientific paper

Sound speed inversions of the Sun show that the profile of the relative difference between the Sun and the standard solar model has a sharp peak around r/Rodot = 0.65, which is the location of the tachocline layer found by rotation inversions. It has been suggested that this sharp peak would be due to the difference, between the Sun and the model, in the hydrogen abundance in the tachocline layer, possibly caused by the weak-mixing process. In this paper, we quantitatively discuss the hydrogen abundance in the tachocline layer based on a seismic solar model, which was constructed using the sound speed and density profiles as well as the depth of the convection zone obtained by helioseismology. One of the important characteristics of the seismic solar model is that it gives us a hydrogen profile as a part of the solution. We find that the hydrogen abundance of the seismic solar model decreases more mildly than that of the standard solar models constructed by i ncorporating the diffusion process. This feature hardly depends on the profile of the heavy elements as well as the uncertainties in the opacity and the equation of state.

Affiliated with

Also associated with

No associations

Rating

Hydrogen Abundance in the Tachocline Layer of the Sun 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 Hydrogen Abundance in the Tachocline Layer of the Sun, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Hydrogen Abundance in the Tachocline Layer of the Sun will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1034902