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Hyperpolarized Xenon for NMR and MRI Applications
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Un enlace binario entre un pulsar de radio y rayos X.

Anne M Archibald1, Ingrid H Stairs, Scott M Ransom

  • 1Department of Physics, McGill University, 3600 Rue University, Montréal, Quebec, H3A 2T8, Canada. aarchiba@physics.mcgill.ca

Science (New York, N.Y.)
|May 23, 2009
PubMed
Resumen
Este resumen es generado por máquina.

Los investigadores detectaron un pulsar de radio milisegundo (MSP) cercano en un sistema binario. Este descubrimiento sugiere que el púlsar ha pasado recientemente de una fase binaria de rayos X de baja masa (LMXB), indicada por la ausencia de un disco de acreción actual.

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Área de la Ciencia:

  • La astronomía y la astrofísica.
  • Objetos compactos Objetos compactos.
  • Los sistemas binarios son sistemas binarios.

Sus antecedentes:

  • Los púlsares de milisegundos (MSP, por sus siglas en inglés) son estrellas de neutrones que giran rápidamente y que se cree que se crean por transferencia de masa de una estrella compañera.
  • Los sistemas binarios de rayos X de baja masa (LMXB) son progenitores teóricos de los MSP, pero los vínculos observacionales directos siguen siendo escurridizos.
  • Las búsquedas anteriores de pulsaciones de radio en LMXBs no han dado detecciones definitivas.

Objetivo del estudio:

  • Para informar de la detección de un nuevo púlsar de radio milisegundos (MSP).
  • Para investigar el estado evolutivo de un sistema MSP cercano con un compañero identificado ópticamente.
  • Explorar la transición de la fase binaria de rayos X de baja masa (LMXB) a la fase de pulsar de radio activo.

Principales métodos:

  • Detección de pulsaciones de radio de un púlsar de milisegundos.
  • Observaciones de seguimiento que incluyen fotometría óptica y espectroscopia.
  • Análisis de datos ópticos para identificar la presencia o ausencia de un disco de acreción.

Principales resultados:

  • Se detectó y observó con éxito un púlsar de radio milisegundos (MSP) cercano.
  • El sistema exhibe una órbita binaria circular con una estrella compañera identificada ópticamente.
  • Las observaciones ópticas indican la reciente desaparición de un disco de acreción, lo que sugiere el cese de la transferencia de masa.

Conclusiones:

  • El MSP de radio detectado probablemente pasó de una fase binaria de rayos X de baja masa (LMXB).
  • La ausencia de un disco de acreción actual apunta a una fase LMXB reciente.
  • Este hallazgo proporciona evidencia observacional para el modelo de spin-up de la formación de pulsares de milisegundos.