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Spin-down de los púlsares de radio milisegundos en el génesis de génesis
1Argelander-Institut für Astronomie, Universität Bonn, Bonn, Germany. tauris@astro.uni-bonn.de
Science (New York, N.Y.)
|February 4, 2012
Resumen
El par de frenado de una estrella de neutrones.
Área de la Ciencia:
- * Astrofísica es la astrofísica.
- * Evolución Estelar de las Estrellas.
- * Física de las estrellas de neutrones
Sus antecedentes:
- * Los púlsares de milisegundos son viejas estrellas de neutrones formadas por la acumulación de masa de un compañero binario.
- * Comprender la evolución temprana del espín requiere analizar la magnetosfera en expansión durante la terminación de la transferencia de masa.
Objetivo del estudio:
- * Para investigar el impacto de la magnetosfera en expansión en la evolución de la estrella de neutrones.
- * Para explicar las diferencias observadas en las distribuciones de espín y las discrepancias de edad en pulsares de milisegundos.
Principales métodos:
- * Se realizaron cálculos de la evolución estelar binaria.
- * Se analizó el par de frenado de las estrellas de neutrones después de la desacoplamiento del lóbulo de Roche de la estrella compañera.
Principales resultados:
- * El par de frenado puede disipar más del 50% de la energía de rotación de un púlsar.
- * Esta disipación de energía puede explicar las diferencias de distribución de espín entre los rayos X y los púlsares de radio.
Conclusiones:
- * El mecanismo del par de frenado es crucial para comprender la evolución de la rotación del pulsar en milisegundos.
- * Este mecanismo puede resolver discrepancias en las distribuciones de espín del púlsar y las estimaciones de edad.
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