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La estructura sísmica del Sol en el Sol

Gough¹, Kosovichev, Toomre

¹D. O. Gough, J. R. Elliott, and T. Sekii are with the Institute of Astronomy, University of Cambridge, CB3 0HA, UK. A. G. Kosovichev and P. R. Giles are with HEPL, Stanford University, Stanford, CA, USA. J. Toomre is at JILA, University of Colorado, Boulder, CO, USA. E. Anderson, J. W. Harvey, F. Hill, and J. W. Leibacher are at the National Solar Observatory, Tucson, AZ, USA. H. M. Antia and S. M. Chitre are at the Tata Institute for Fundamental Research, Bombay, India. S. Basu and J. Christensen-Dalsgaard are at the Theoretical Astrophysics Centre, Aarhus University, Denmark. B. Chaboyer is at the Canadian Institute for Theoretical Astrophysics, Toronto, Canada. W. A. Dziembowski is at the Copernicus Astronomical Center, Warsaw, Poland. A. Eff-Darwich is at the Instituto Astrofisico de Canarias, Tenerife, Canary Islands. P. R. Goode is at the New Jersey Institute of Technology, Newark, NJ, USA. J. A. Guzik is at the Los Alamos National Laboratory, Los Alamos, NM, USA. M. J. P. F. G. Monteiro is at the University of Oporto, Postugal. O. Richard and S. Vauclair are at the Observatoire Midi-Pyrenees, Toulouse, France. H. Shibahashi and M. Takata are in the Department of Astronomy, University of Tokyo, Tokyo, Japan. M. J. Thompson and S. V. Vorontsov are at Queen Mary and Westfield College, University of London, London, UK.

Science (New York, N.Y.)

|May 31, 1996

Resumen

Los datos de la helioseismología muestran que la estructura interna del sol se alinea con los modelos estándar, pero con variaciones más suaves de la velocidad del sonido cerca del núcleo. Esto sugiere posibles inexactitudes en los modelos solares con respecto a la composición química o el movimiento interno.

Área de la Ciencia:

Física solar Física solar es la física de la energía solar.
La helioseismología.
El modelado astrofísico.

Sus antecedentes:

La estructura interna del Sol es crucial para comprender la física estelar.
Los modelos solares estándar son ampliamente utilizados, pero pueden tener limitaciones.

Objetivo del estudio:

Para comparar la estructura interna del Sol con un modelo estándar calibrado utilizando datos de helioseismología.
Para identificar discrepancias e investigar sus posibles causas.

Principales métodos:

Análisis de los datos del Grupo de la Red de Oscilación Global (GONG).
Comparación de las variaciones observadas de la velocidad del sonido con las predicciones de un modelo solar estándar.

Principales resultados:

Los datos de la helioseismología generalmente concuerdan con el modelo solar estándar.
Se observó una variación más suave de la velocidad del sonido en el Sol debajo de la zona de convección en comparación con el modelo.
Esta discrepancia puede deberse a inexactitudes en el modelado de asentamientos gravitacionales o movimientos macroscópicos no modelados.

Conclusiones:

Los hallazgos destacan las áreas potenciales de mejora en los modelos solares, específicamente con respecto a la inhomogeneidad química y la dinámica interna.
El conocimiento preciso de la estructura solar ayuda a comprender la física fundamental (opacidad, ecuación de estado, movimiento de ondas) aplicable a toda la astrofísica.

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