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Estructura térmica fina de una región activa coronal
Fabio Reale1, Susanna Parenti, Kathy K Reeves
1Dipartimento di Scienze Fisiche ed Astronomiche, Sezione di Astronomia, Università di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy. reale@astropa.unipa.it
Science (New York, N.Y.)
|December 8, 2007
Resumen
El estudio de la corona solar.
Área de la Ciencia:
- Física solar Física solar es la física de la energía solar.
- La física del plasma es la física del plasma.
- La astrofísica es la astrofísica.
Sus antecedentes:
- La comprensión de los mecanismos de calentamiento de la corona solar es crucial.
- La estructura térmica de la corona solar proporciona información clave para el diagnóstico.
Objetivo del estudio:
- Para determinar la estructura térmica fina de la corona solar.
- Para limitar los mecanismos de calentamiento de la corona solar utilizando técnicas avanzadas de imagen.
Principales métodos:
- Utilizó el telescopio de rayos X Hinode para obtener imágenes de la corona solar.
- Empleó múltiples bandas de paso y combinaciones de filtros para el diagnóstico de temperatura.
- Analizó las relaciones de energía de las imágenes tomadas en cinco filtros diferentes.
Principales resultados:
- Reveló una corona solar altamente estructurada térmicamente en una región activa.
- Se observaron estructuras térmicas muy finas en el núcleo y estructuras más grandes periféricamente.
- Se detectó una distribución térmica continua a lo largo de bucles coronales y estructuras entrelazadas.
- Se encontraron variaciones en la estructuración térmica a lo largo de la línea de visión.
Conclusiones:
- Las estructuras térmicas finas observadas son esenciales para comprender el calentamiento coronal.
- Las imágenes con múltiples filtros proporcionan información detallada sobre las complejas propiedades térmicas de la corona solar.
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