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La transformación de una estrella en un planeta en un milisegundo en un pulsar binario
M Bailes1, S D Bates, V Bhalerao
1Centre for Astrophysics and Supercomputing and ARC Centre for All-Sky Astrophysics (CAASTRO), Swinburne University of Technology, Post Office Box 218 Hawthorn, VIC 3122, Australia. mbailes@swin.edu.au
Science (New York, N.Y.)
|August 27, 2011
Resumen
Los investigadores descubrieron que un solitario púlsar de milisegundos, PSR J1719-1438, está en realidad en un sistema binario. Su compañera puede ser una enana blanca de carbono de masa ultra baja, que ofrece pistas sobre los orígenes de los púlsares.
Área de la Ciencia:
- La astronomía y la astrofísica.
- Objetos compactos Objetos compactos.
- Las estrellas de neutrones son estrellas de neutrones.
Sus antecedentes:
- Los púlsares de milisegundos (MSP) son estrellas de neutrones de rápida rotación, que generalmente se encuentran en sistemas binarios donde la acreción los hace girar hacia arriba.
- Una fracción significativa (alrededor del 30%) de los MSP son solitarios, lo que plantea un desafío para el modelo de formación estándar.
- Comprender el origen de los MSP solitarios es crucial para obtener una imagen completa de la evolución estelar.
Objetivo del estudio:
- Para investigar la naturaleza y el origen del solitario púlsar de milisegundos PSR J1719-1438.8.
- Para determinar si PSR J1719-1438 es verdaderamente solitario o parte de un sistema binario.
- Para caracterizar el objeto compañero y sus implicaciones para la evolución del púlsar.
Principales métodos:
- Utilizando datos de la encuesta del radiotelescopio Parkes de 64 metros.
- Realizar análisis de tiempo de la señal del púlsar para detectar variaciones orbitales.
- Cálculo de la masa y densidad del objeto compañero basado en parámetros orbitales.
Principales resultados:
- El púlsar de milisegundos PSR J1719-1438 fue detectado en un sistema binario con un período orbital de 2,2 horas.
- La masa de la compañera es comparable a la de Júpiter.
- La alta densidad de la compañera (mínimo 23 g/cm3) sugiere que se trata de una enana blanca de carbono de muy baja masa.
Conclusiones:
- El descubrimiento desafía la naturaleza solitaria de algunos MSP y proporciona evidencia de vías de formación binaria.
- Las propiedades de la compañera sugieren un pasado como un binario de rayos X ultracompacto de baja masa.
- Este sistema ofrece información sobre la evolución extrema de las estrellas binarias y la supervivencia de las compañeras durante las fases de acreción.
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