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¿Cometas de corto período: cuerpos primordiales o fragmentos de colisión?
1P. Farinella, Dipartimento di Matematica, Universita di Pisa, Via Buonarroti 2, 56127 Pisa, Italy. D. R. Davis, Planetary Science Institute, 620 North Sixth Avenue, Tucson, AZ 85705-8331, USA.
Science (New York, N.Y.)
|August 16, 1996
Resumen
Las colisiones entre los objetos del cinturón de Edgeworth-Kuiper (EKOs) dan forma a su población y crean cometas de corto período. Los EKO más pequeños se rompen con frecuencia, lo que influye en las propiedades del cometa, como la forma y el color.
Área de la Ciencia:
- Ciencias planetarias Ciencias planetarias.
- La astronomía es la astronomía.
- La astrofísica es la astrofísica.
Sus antecedentes:
- El Cinturón Edgeworth-Kuiper (EKB) es una vasta región más allá de Neptuno poblada por numerosos cuerpos pequeños.
- Estos objetos, conocidos como Edgeworth-Kuiper Belt Objects (EKOs), son cruciales para comprender la evolución del sistema solar.
- Sus descendientes, los cometas de corto período, proporcionan información sobre la composición del sistema solar interior.
Objetivo del estudio:
- Investigar el papel de los procesos de colisión en la formación de la población del cinturón Edgeworth-Kuiper.
- Determinar cómo las colisiones influyen en la formación y las características de los cometas de corto período.
- Para explicar las propiedades físicas de los cometas de corto período basado en su origen.
Principales métodos:
- Utilizó un avanzado modelado computacional para simular colisiones entre EKOs.
- Analizó la distribución de tamaño y frecuencia de los fragmentos resultantes de la ruptura de colisión.
- Se investigaron las vías dinámicas para que los EKO ingresen al sistema solar interno a través de resonancias.
Principales resultados:
- Las colisiones son un proceso dominante para los EKO de menos de 100 km, lo que lleva a la ruptura frecuente y una distribución de tamaño de la ley de poder.
- Los EKO más grandes (>100 km) generalmente sobreviven a la edad del sistema solar.
- Las colisiones inyectan plausiblemente EKOs de 1-10 km en resonancias, facilitando su transporte al sistema solar interior como cometas.
Conclusiones:
- La evolución de la colisión es fundamental para comprender el Cinturón Edgeworth-Kuiper.
- La naturaleza fragmentaria de los EKOs explica las propiedades físicas observadas de los cometas de corto período.
- Esta investigación proporciona un modelo cohesivo que vincula la dinámica de EKO, las colisiones y las características de los cometas.
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