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The process of element segregation in stars (also called "microscopic diffusion") has to be introduced in all computations of stellar structure to obtain consistent models. Although recognized by the pioneers of stellar physics, this process has long been forgotten, except for white dwarfs and for the so-called "chemically peculiar stars". More recently helioseismology has given evidence that this process occurs in the Sun, and leads to helium and heavier element depletion by about 20 percent. Some macroscopic motions (mild mixing) must also occur below the convection zone in order to account for the lithium depletion. These motions do not prevent the segregation : they only slightly smooth the abundance gradients. These results are presented here and the connexion with the 3He abundance is discussed. The importance of these processes for Pop II stars is also developped. 相似文献
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Sylvie Vauclair 《Space Science Reviews》1998,85(1-2):71-78
Element settling inside the Sun now becomes detectable from the comparison of the observed oscillation modes with the results
of the theoretical models. This settling is due, not only to gravitation, but also to thermal diffusion and radiative acceleration
(although this last effect is small compared to the two others). It leads to abundance variations of helium and heavy elements
of ≅ 10% below the convective zone. Although not observable from spectroscopy, such variations lead to non-negligible modifications
of the solar internal structure and evolution. Helioseismology is a powerful tool to detect such effects, and its positive
results represent a great success for the theory of stellar evolution. Meanwhile, evidences are obtained that the element
settling is slightly smoothed down, probably due to mild macroscopic motions below the convective zone. Additional observations
of the abundances of both 7Li and 3He lead to specific constraints on these particular motions.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
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