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The Solar Rotation Rate Ω(R, θ)

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Abstract

In recent years, the capability to detect and analyse solar oscillation acoustic modes has greatly improved. The development of ground based networks like GONG or BiSON and the use of space platforms like SOHO has allowed us to study the structure and dynamics of the Sun with unprecedented precision.

In this work we explore the distribution of the rotation in the solar interior, specially in the core. This kind of information is essential in order to study the physical processes involved in the evolution of the Sun and many other stars.

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Authors and Affiliations

  1. Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA, 02139, USA

    A. Eff-Darwich & S.G. Korzennik

  2. Instituto de Astrofísica de Canarias C/Via Láctea, s/n, La Laguna, Tenerife, 38205, Spain

    T. Roca Cortés, F. Pérez Hernández & P. Pallé

Authors
  1. A. Eff-Darwich
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  2. S.G. Korzennik
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  3. T. Roca Cortés
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  4. F. Pérez Hernández
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  5. P. Pallé
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Eff-Darwich, A., Korzennik, S., Cortés, T.R. et al. The Solar Rotation Rate Ω(R, θ). Astrophysics and Space Science 263, 347–350 (1998). https://doi.org/10.1023/A:1002103822548

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  • DOI: https://doi.org/10.1023/A:1002103822548

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