skip to main content
Idioma:
Primo Search
Clear Search Box
Search in: Busca Geral
Busca Avançada
Busca por Índices

Correlation between the photon index and X-ray luminosity of black hole X-ray binaries and active galactic nuclei: observations and interpretation

Yang, Qi-Xiang ; Xie, Fu-Guo ; Yuan, Feng ; Zdziarski, Andrzej A ; Gierliński, Marek ; Ho, Luis C ; Yu, Zhaolong

Monthly notices of the Royal Astronomical Society, 2015-02, Vol.447 (2), p.1692-1704 [Periódico revisado por pares]

London: Oxford University Press

Texto completo disponível

Citações Citado por
  • Título:
    Correlation between the photon index and X-ray luminosity of black hole X-ray binaries and active galactic nuclei: observations and interpretation
  • Autor: Yang, Qi-Xiang ; Xie, Fu-Guo ; Yuan, Feng ; Zdziarski, Andrzej A ; Gierliński, Marek ; Ho, Luis C ; Yu, Zhaolong
  • Assuntos: Accretion disks ; Active galactic nuclei ; Binary stars ; Black holes ; Black holes (astronomy) ; Correlation ; Correlation analysis ; Luminosity ; Photons ; Star & galaxy formation ; X-ray astronomy ; X-ray stars ; X-rays
  • É parte de: Monthly notices of the Royal Astronomical Society, 2015-02, Vol.447 (2), p.1692-1704
  • Notas: ObjectType-Article-1
    SourceType-Scholarly Journals-1
    ObjectType-Feature-2
    content type line 23
  • Descrição: We investigate the observed correlation between the 2–10 keV X-ray luminosity (in unit of the Eddington luminosity; l X ≡ L X/L Edd) and the photon index (Γ) of the X-ray spectrum for both black hole X-ray binaries (BHBs) and active galactic nuclei (AGNs). We construct a large sample, with 10− 9 ≲ l X ≲ 10− 1. We find that Γ is positively and negatively correlated with l X when l X ≳ 10− 3 and 10− 6.5 ≲ l X ≲ 10− 3, respectively, while Γ is nearly a constant when l X ≲ 10− 6.5. We explain the above correlation in the framework of a coupled hot accretion flow–jet model. The radio emission always comes from the jet while the X-ray emission comes from the accretion flow and jet when l X is above and below 10−6.5, respectively. More specifically, we assume that with the increase of mass accretion rate, the hot accretion flow develops into a clumpy and further a disc–corona two-phase structure because of thermal instability. We argue that such kind of two-phase accretion flow can explain the observed positive correlation.
  • Editor: London: Oxford University Press
  • Idioma: Inglês
Voltar para lista de resultados
Ir para página anteriorAnterior Resultado  8 AvançarIr para próxima página

  • Realização: ABCD-USP USP   Logos de Redes Sociais: Freepik

Buscando em bases de dados remotas. Favor aguardar.