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La evolución temprana del sistema solar interno: una perspectiva meteorítica
C M O'D Alexander1, A P Boss, R W Carlson
1Department of Terrestrial Magnetism, Carnegie Institution of Washington, 5241 Broad Branch Road, N.W., Washington, DC 20015, USA.
Science (New York, N.Y.)
|July 7, 2001
Resumen
El sistema solar es el sistema solar.
Área de la Ciencia:
- Ciencias planetarias Ciencias planetarias.
- La astrofísica es la astrofísica.
- Cosmoquímica es la cosmoquímica.
Sus antecedentes:
- Teorías de la formación del sistema solar teorías de la formación del sistema solar
- La evolución temprana del sistema solar en la evolución del sistema solar.
- Composición y origen de los meteoritos.
Objetivo del estudio:
- Investigar los orígenes de los sólidos del sistema solar.
- Determinar los mecanismos de formación de los meteoritos.
- Reconstruir la línea de tiempo de los primeros procesos del sistema solar.
Principales métodos:
- Análisis de la composición del meteorito.
- Datamiento radiométrico de los materiales del sistema solar.
- Modelado de la evolución del disco protoplanetario.
Principales resultados:
- Los radionúclidos de corta vida en los meteoritos sugieren la irradiación de partículas energéticas.
- Las inclusiones y cóndrulas ricas en calcio y aluminio probablemente se formaron en el cinturón de asteroides.
- Los meteoritos condríticos se formaron en los discos de T Tauri, reteniendo potencialmente la memoria de las temperaturas más altas.
Conclusiones:
- El agua de la Tierra probablemente se originó en asteroides portadores de agua o planetesimales helados cerca de Júpiter.
- La formación de planetas terrestres ocurrió después de la dispersión de la nebulosa solar.
- La evolución del sistema solar involucró la formación de discos, chorros bipolares y la posterior diferenciación.
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