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¹F. Hill, E. R. Anderson, J. W. Harvey, R. P. Hubbard, J. R. Kennedy, J. W. Leibacher, J. A. Pintar, C. G. Toner, R. Toussaint, and W. E. Williams are with the National Solar Observatory, National Optical Astronomy Observatories (NOAO), Post Office Box 26732, Tucson, AZ 85726-6732, USA. P. B. Stark is with the Department of Statistics and Space Sciences Laboratory, University of California, Berkeley, CA 94720, USA. R. T. Stebbins and D. A. Haber are with JILA, University of Colorado, Boulder, CO 80309, USA. H. M. Antia is with the Tata Institute of Fundamental Research, Bombay, India. T. M. Brown and S. Tomczyk are with the High Altitude Observatory, National Center for Atmospheric Research, Boulder, CO 80307, USA. T. L. Duvall is with the NASA Goddard Space Flight Center, Stanford University, Center for Space Science and Astrophysics (CSSA), Stanford, CA 94305, USA. D. H. Hathaway is with the NASA Marshall Space Flight Center, Mail Code ES82, Huntsville, AL 35812, USA. R. Howe and M. J. Thompson are with the Astronomy Unit, Queen Mary and Westfield College, London E1 4NS, UK. H. P. Jones is with the NASA Goddard Space Flight Center Southwest Station, NOAO, Tucson, AZ 85726, USA. S. G. Korzennik is with the Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA. A. G. Kosovichev and J. Schou are with Stanford University, CSSA, Stanford, CA 94305, USA. K. G. Libbrecht is with the California Institute of Technology, 264-33, Pasadena, CA 91125, USA. E. J. Rhodes is with the Department of Physics and Astronomy, University of Southern California, Los Angeles, CA 90089, USA.

Science (New York, N.Y.)

|May 31, 1996

Resumen

El proyecto Global Oscillation Network Group (GONG) mide con precisión las resonancias acústicas solares, proporcionando datos detallados sobre la actividad solar. Estos hallazgos mejoran nuestra comprensión de la estructura interna y la dinámica del Sol.

Área de la Ciencia:

La helioseismología.
Física solar Física solar es la física de la energía solar.
Asteroseismología La Asteroseismología

Sus antecedentes:

Las resonancias acústicas del Sol ofrecen información sobre su estructura interna y dinámica.
Estudios heliosísmicos anteriores han proporcionado datos valiosos, aunque a veces diferentes.

Objetivo del estudio:

Para estimar las frecuencias, amplitudes y anchos de línea de las resonancias acústicas solares utilizando los datos del Grupo de la Red de Oscilación Global (GONG).
Evaluar la precisión y las posibles discrepancias de las mediciones de GONG en comparación con otros conjuntos de datos heliosísmicos.

Principales métodos:

Análisis de conjuntos de datos solares de 36 días del proyecto GONG.
Estimación de los parámetros de resonancia acústica, incluidas las frecuencias, amplitudes y anchos de línea.
El promedio de frecuencias sobre el orden azimutal (m) para mejorar la resolución y reducir los errores.

Principales resultados:

Se estima que hay más de 250.000 resonancias acústicas solares.
Se logró una resolución de frecuencia de 0.321 microhertz para conjuntos de datos individuales.
El error formal medio es de 0,044 microhertz y el error fraccionario es de 1,6 x 10^-5 para frecuencias m-promediadas.
Error fraccionario proyectado de 3 x 10^-6 para un conjunto de datos de 3 años.
Diferencias observadas de 0,03 a 0,08 microhertz entre GONG y otros conjuntos de datos heliosísmicos.

Conclusiones:

El proyecto GONG proporciona mediciones de alta precisión de las resonancias acústicas solares.
Las discrepancias con otros conjuntos de datos pueden deberse a errores sistemáticos, errores aleatorios o cambios reales en la estructura solar.
Los hallazgos contribuyen a una comprensión más precisa de la dinámica solar y los procesos internos.

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