The abundance of He-3 in the solar wind - A constraint for models of solar evolution

Details The abundance of He-3 in the solar wind - A constraint for models of solar evolution The abundance of He-3 in the solar wind - A constraint for models of solar evolution

Jul 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990soph..128..203b&link_type=abstract

(IAU, The Inside the Sun Colloquium, 121st, Versailles, France, May 22-26, 1989) Solar Physics (ISSN 0038-0938), vol. 128, July

Physics

15

Abundance, Helium Isotopes, Solar Atmosphere, Solar Interior, Solar Wind, Solar Corona, Spaceborne Experiments, Stellar Evolution, Stellar Models, Transport Theory, Turbulent Diffusion

Scientific paper

He-3 abundance measurements have been performed under a large variety of solar wind conditions, and refined models have been developed for the transport processes in the chromosphere and the transition region and for the processes occurring in the solar corona. From these measurements the present isotopic number ratio He-3/H-4 is estimated to be (4.1 + or - 1.0) x 10 to the -4th at the solar surface. The zero-age Main-Sequence abundance of He-3 (after burning of D) might have been slightly lower (by about 10 to 20 percent) than the present-day value. Nonstandard solar models involving mild turbulent diffusion (Lebreton and Maeder, 1987) could account for a slow secular increase of the He-3/He-4 ratio in the solar atmosphere. On the other hand it is difficult to reconcile models with severe mass loss as proposed by Guzik et al. (1987) with this constraint. The slowing down of the solar rotation during the early Main-Sequence evolution was accompanied by stronger differential rotation probably implying a more effective mixing of the inner parts. Again, the surface abundance of He-3 imposes severe limits on the evolution of the distribution of momentum within the early sun.

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