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Astron. Astrophys. 364, 876-878 (2000)

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2. The solar rotation profile

Through the inversion of LOWL frequency-splitting data spanning 2 years, Charbonneau et al. (1998) have derived the following internal solar rotation rate for [FORMULA]:

[EQUATION]

The observed latitudinal differential rotation [FORMULA] is expressed as:

[EQUATION]

The parameters values are: [FORMULA] nHz, [FORMULA] nHz, [FORMULA] nHz, [FORMULA] nHz; [FORMULA] is the radius at the bottom of the solar convective zone and [FORMULA] the tachocline thickness. Similar expressions can be found in the literature e.g. Li & Wilson (1998), Corbard et al. (1998), Antia et al. (1998). The fact that [FORMULA] is almost constant at greater depth is in conflict with earlier predictions of a faster rotating core (Pinsonneault et al. 1989; Zahn 1992), and it rules out that angular momemtum be transported vertically through shear-induced turbulence. But this possibility still exists in the shear flow of the tachocline.

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© European Southern Observatory (ESO) 2000

Online publication: January 29, 2001
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