期刊
ASTRONOMY & ASTROPHYSICS
卷 368, 期 2, 页码 L8-L12出版社
EDP SCIENCES S A
DOI: 10.1051/0004-6361:20010145
关键词
stars : interiors; stars : oscillations; stars : rotation
Helioseismic inversions for the rotation rate have established the presence of a tachocline near the base of the solar convection zone. We show that the tachocline produces a characteristic oscillatory signature in the splitting coefficients of low degree modes, which could he observed on distant stars. Using this signature it may be possible to determine the characteristics of the tacholine using only low degree modes. The limitations of this technique in terms of observational uncertainties are discussed, to assess the possibility of detecting tachoclines on distant stars.
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