Astronomy and Astrophysics – Astrophysics – High Energy Astrophysical Phenomena
Scientific paper
2010-06-26
Astronomy and Astrophysics
Astrophysics
High Energy Astrophysical Phenomena
Accepted for publication in the Astrophysical Journal
Scientific paper
We present an analysis of the broad-band spectra of 4U~1705--44 obtained with {\it Suzaku} in 2006--2008 and by {\it BeppoSAX} in 2000. The source exhibits two distinct states: the hard state shows emission from 1 to 150 keV, while the soft state is mostly confined to be $<40$ keV. We model soft-state continuum spectra with two thermal components, one of which is a multicolor accretion disk and the other is a single-temperature blackbody to describe the boundary layer, with additional weak Comptonization represented by either a simple power law or the SIMPL model by Steiner et al. The hard-state continuum spectra are modeled by a single-temperature blackbody for the boundary layer plus strong Comptonization, modeled by a cutoff power law. While we are unable to draw firm conclusions about the physical properties of the disk in the hard state, the accretion disk in the soft state appears to approximately follow $L\propto T^{3.2}$. The deviation from $L\propto T^4$, as expected from a constant inner disk radius, might be caused by a luminosity-dependent spectral hardening factor and/or real changes of the inner disk radius in some part of the soft state. The boundary layer apparent emission area is roughly constant from the hard to the soft states, with a value of about 1/11 of the neutron star surface. The magnetic field on the surface of the NS in 4U~1705--44 is estimated to be less than about $1.9\times 10^8$ G, assuming that the disk is truncated by the ISCO or by the neutron star surface. Broad relativistic Fe lines are detected in most spectra and are modeled with the diskline model. The strength of the Fe lines is found to correlate well with the boundary layer emission in the soft state. In the hard state, the Fe lines are probably due to illumination of the accretion disk by the strong Comptonization emission.
Homan Jeroen
Lin Dacheng
Remillard Ronald A.
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