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Updated: Oct 31, 2025
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A 100 KW Class Applied-field Magnetoplasmadynamic Thruster
Published on: December 22, 2018
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Una enana blanca altamente magnetizada y de rápida rotación tan pequeña como la Luna
Ilaria Caiazzo1, Kevin B Burdge2, James Fuller2
1Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA, USA. ilariac@caltech.edu.
Nature
|July 1, 2021
Resumen
Los investigadores descubrieron una estrella enana blanca extrema, ZTF J190132.9+145808.7, resultado de una fusión. Esta estrella giratoria y altamente magnetizada tiene un radio cercano al límite de Chandrasekhar, lo que sugiere procesos de enfriamiento únicos.
Área de la Ciencia:
- Astronomía y astrofísica
- Evolución estelar
- Objetos compactos
Sus antecedentes:
- Las enanas blancas son la etapa evolutiva final para las estrellas menos masivas que ocho masas solares.
- Las enanas blancas se observan con frecuencia en sistemas binarios, donde las interacciones gravitacionales pueden conducir a fusiones.
- Las fusiones pueden dar lugar a supernovas de tipo Ia o remanentes masivos de enanas blancas.
Objetivo del estudio:
- Para reportar el descubrimiento y la caracterización de una enana blanca excepcionalmente extrema.
- Para investigar las propiedades de las enanas blancas formadas por fusiones estelares.
- Para entender los procesos físicos que ocurren en los restos estelares altamente densos y magnetizados.
Principales métodos:
- Astronomía observacional que utiliza telescopios avanzados para detectar y analizar objetos celestes.
- Análisis espectroscópico para determinar las propiedades estelares, como la intensidad del campo magnético y el período de rotación.
- Mediciones fotométricas para restringir el radio y la masa estelares.
Principales resultados:
- Descubrimiento de la enana blanca ZTF J190132.9+145808.7 con propiedades extremas.
- Período de rotación medido de 6,94 minutos.
- La intensidad del campo magnético superficial observada está entre 600 y 900 mega gauss.
- El radio estelar es solo ligeramente más grande que la Luna, lo que implica una masa cerca del límite de Chandrasekhar.
Conclusiones:
- Las propiedades observadas sugieren que ZTF J190132.9+145808.7 es un remanente de una fusión de enanas blancas.
- Las características extremas de la estrella, incluido el giro rápido y el alto campo magnético, son consistentes con los procesos de dínamo inducidos por la fusión.
- La alta densidad probablemente impulsa el enfriamiento a través de los procesos de Urca.
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