J. Phys. Colloques
Volume 49, Numéro C1, Mars 1988IAU Colloquium N° 102 on UV and X-ray Spectroscopy of Astrophysical and Laboratory Plasmas
|Page(s)||C1-47 - C1-50|
J. Phys. Colloques 49 (1988) C1-47-C1-50
IRON K-LINE EMISSION FROM X-RAY BINARIESK. MASAI1, S. HAYAKAWA2 et F. NAGASE2
1 Institute of Plasma Physics, Nagoya 464, Japan
2 Department of Astrophysics, Nagoya University, Nagoya 464, Japan
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.