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Estructuras y variaciones espectrales de la heliosfera exterior en mapas de átomos energéticamente neutros del IBEX
H O Funsten1, F Allegrini, G B Crew
1Los Alamos National Laboratory, Los Alamos, NM 87545, USA. hfunsten@lanl.gov
Science (New York, N.Y.)
|October 17, 2009
Resumen
El Explorador de Límites Interestelares (IBEX) reveló distintas poblaciones de protones energéticos en la cubierta heliosférica. Una característica prominente de la cinta, probablemente cerca del campo magnético interestelar local, muestra una presión iónica significativamente más alta que la población distribuida globalmente.
Área de la Ciencia:
- Física del espacio Física del espacio
- Heliofísica es la heliofísica.
- La astrofísica es la astrofísica.
Sus antecedentes:
- La heliosfera es la región entre el choque de terminación del viento solar y el medio interestelar local.
- Los átomos neutros energéticos (ENAs) proporcionan información sobre las condiciones plasmáticas en la cubierta heliogénica.
Objetivo del estudio:
- Para analizar imágenes de todo el cielo de ENAs de la heliosfera obtenidas por el Explorador de Límites Interestelares (IBEX).
- Para caracterizar las poblaciones de protones energéticos y su distribución espacial dentro de la heliosfera.
Principales métodos:
- Utilizando mapas de flujo de ENA de todo el cielo de IBEX.
- Analizando las firmas espectrales de las poblaciones de protones heliosheath en el rango de 0,2 a 6 kilovoltios de electrones.
Principales resultados:
- Se identificaron distintas poblaciones de protones heliosheath no térmicos con firmas espectrales correlacionadas con la latitud eclíptica.
- Se observó una población globalmente distribuida de protones calentados por el choque de terminación.
- Detectó una característica parecida a una cinta, un arco en el cielo, probablemente cerca de la dirección local del campo magnético interestelar.
- Cuantificó el producto de la presión de iones no térmicos y el espesor de la cinta (70-100 pN/cm2 AU), superando significativamente el de la población distribuida globalmente (30-60 pN/cm2 AU).
Conclusiones:
- La heliosfera contiene complejas poblaciones de protones energéticos, incluida una característica de cinta dominante.
- La presión iónica más alta de la cinta sugiere un proceso físico o interacción distinta dentro de la hélioesfera.
- Las observaciones IBEX proporcionan datos cruciales para comprender la interacción de la heliosfera con el medio interestelar local.
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