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1988•Le Journal de Physique ColloquesOpen access

IRON K-LINE EMISSION FROM X-RAY BINARIES

K. Masai, S. Hayakawa, F. Nagase

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Abstract

Emission mechanisms of the iron Kα-lines in X-ray binaries are discussed in relation with the characteristic temperature Tx of continuum radiation thereof. The 6.7 keV line is ascribed to radiative recombination followed by cascades in a corona of ~ 100 eV formed above the accretion disk. This mechanism is attained for Tx ≤ 10 keV as observed for low mass X-ray binaries. The 6.4 keV line observed for binary X-ray pulsars with Tx > 10 keV is likely due to fluorescence outside the He II ionization front.

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Emission mechanisms of the iron Kα-lines in X-ray binaries are discussed in relation with the characteristic temperature Tx of continuum radiation thereof. The 6.7 keV line is ascribed to radiative recombination followed by cascades in a corona of ~ 100 eV formed above the accretion disk. This mechanism is attained for Tx ≤ 10 keV as observed for low mass X-ray binaries. The 6.4 keV line observed for binary X-ray pulsars with Tx > 10 keV is likely due to fluorescence outside the He II ionization front.

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Available abstract

Emission mechanisms of the iron Kα-lines in X-ray binaries are discussed in relation with the characteristic temperature Tx of continuum radiation thereof. The 6.7 keV line is ascribed to radiative recombination followed by cascades in a corona of ~ 100 eV formed above the accretion disk. This mechanism is attained for Tx ≤ 10 keV as observed for low mass X-ray binaries. The 6.4 keV line observed for binary X-ray pulsars with Tx > 10 keV is likely due to fluorescence outside the He II ionization front.

Key concepts: Line (geometry), X-ray, Astrophysics, Emission spectrum, Physics, Astronomy, Materials science, Optics

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