Abstract
The second-order asymptotic theory for low-degree, higher-order p-modes is seen to be inadequate to reproduce frequency separations D n,ℓ for the low-degree p-modes in the solar 5 min-oscillations in a satisfactory way. The reason of the inadequacy is that the inner boundary of the resonant acoustic cavity in the Sun is supposed to be located close to the solar centre, while this condition is not really fulfilled for the oscillations concerned. Therefore, a first-order asymptotic theory for p-modes is developed for which the inner boundary of the resonant acoustic cavity is situated at larger distances from the star’s centre. This theory applies to low-degree p-modes of less high radial orders and to intermediate-degree p-modes as well. Its validity is verified for the compressible equilibrium sphere of uniform mass density.
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Notes
- 1.
This section is a reproduction of Van Hoolst, T., Smeyers, P.: The quantities D n,ℓ as measures of small frequency separations in the Sun and their origin. Astronomy & Astrophysics 248, 647–655 (1991). With permission from Astronomy & Astrophysics, http://www.aanda.org.
- 2.
The remaining part of this chapter is partially a reproduction of Smeyers, P.: Asymptotic representation of low- and intermediate-degree p-modes in stars. Astronomy & Astrophysics 407, 643–653 (2003). With permission from Astronomy & Astrophysics, http://www.aanda.org.
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Smeyers, P. (2010). Asymptotic Representation of Low-Degree and Intermediate-Degree p-Modes. In: Linear Isentropic Oscillations of Stars. Astrophysics and Space Science Library, vol 371. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-642-13030-4_16
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DOI: https://doi.org/10.1007/978-3-642-13030-4_16
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