Thermal iron Kα line emission from the X-ray binary GX 339-4

Details Thermal iron Kα line emission from the X-ray binary GX 339-4 Thermal iron Kα line emission from the X-ray binary GX 339-4

Aug 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003newa....8..575x&link_type=abstract

New Astronomy, Volume 8, Issue 6, p. 575-580.

Physics

Black Hole Physics, Stars: Individual: Gx 339-4, X-Rays: Stars

Scientific paper

The accretion rate of the black hole candidate X-ray binary GX 339-4 in the `off' state is low, and an advection dominated accretion flow (ADAF) is present. Hydrogen-like and helium-like iron Kα emission lines at 6.7 and 6.95 keV from hot plasma of ADAF can be produced by recombination-cascade processes with moderately high intensities, which are markedly distinguished from the fluorescent iron Kα line at ~6.4 keV. We show that the observational features of GX 339-4 can be explained by the ADAF model, if the iron abundance is more than 10 times the solar value, though the reason for such a high abundance is still unclear. We suggest that the increase of the accretion rate makes GX 339-4 change from off, low, intermediate, to high and very high states, and the line center of iron Kα will therefore shift from ~6.83 to ~6.4 keV, i.e. to the fluorescent disc-line, since the disappearance of the ADAF due to its high accretion rate.

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