Volume 384, Number 2, MarchIII 2002
|Page(s)||666 - 677|
|Section||Planets and planetary systems|
|Published online||15 March 2002|
Inferences on the solar envelope with high-degree modes
Osservatorio Astrofisico di Catania, Via S. Sofia 78, 95123 Catania, Italy
2 Teoretisk Astrofysik Center, Danmarks Grundforskningsfond, 8000 Aarhus C, Denmark
3 Institut for Fysik og Astronomi, Aarhus Universitet, Ny Munkegade bygn. 520, 8000 Aarhus C, Denmark e-mail: firstname.lastname@example.org
4 Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305, USA e-mail: csoares@tucano.Stanford.EDU
5 Astronomy Department, Yale University, New Haven CT 06520-8101, USA e-mail: email@example.com
Corresponding author: M. P. Di Mauro, firstname.lastname@example.org
Accepted: 4 January 2002
We investigate the structure of the Sun by helioseismic inversion of a set of p-mode frequencies which includes new precise observations of modes with high degree () obtained from the MDI instrument on the SOHO satellite (Rhodes et al. [CITE]). Such data have the potential to improve the resolution of the solar structure in the near-surface region, to provide detailed tests of the equation of state and constrain the envelope helium abundance. In order to suppress the uncertainties in the treatment of the surface layers in helioseismic inversion procedures, we introduce here the use of a new surface term, developed on the basis of higher-order asymptotic theory of acoustic modes and suitable for the handling of high-degree mode frequencies.
Key words: Sun: helioseismology / Sun: interior
© ESO, 2002
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