* Astronomy

Title: XTE J1701-462 and its Implications for the Nature of Subclasses in Low-Magnetic-Field Neutron Star Low-Mass X-Ray Binaries
Authors: Jeroen Homan, Michiel van der Klis, Joel K. Fridriksson, Ronald A. Remillard, Rudy Wijnands, Mariano Mendez, Dacheng Lin, Diego Altamirano, Piergiorgio Casella, Tomaso Belloni, Walter H. G. Lewin

We report on an analysis of RXTE data of the transient neutron star low-mass X-ray binary (NS-LMXB) XTE J1701-462, obtained during its 2006-2007 outburst. The X-ray properties of the source changed between those of various types of NS-LMXB subclasses. At high luminosities the source switched between two types of Z source behaviour and at low luminosities we observed a transition from Z source to atoll source behaviour. These transitions between subclasses primarily manifest themselves as changes in the shapes of the tracks in X-ray colour-colour and hardness-intensity diagrams, but they are accompanied by changes in the kHz quasi-periodic oscillations, broad-band variability, burst behaviour, and/or X-ray spectra. We find that the low-energy X-ray flux is a good parameter to track the gradual evolution of the tracks in colour-colour and hardness-intensity diagrams, allowing us to resolve the evolution of the source in greater detail than before and relate the observed properties to other NS-LMXBs. We further find that during the transition from Z to atoll, characteristic behaviour known as the atoll upper banana can equivalently be described as the final stage of a weakening Z source flaring branch, thereby blurring the line between the two subclasses. Our findings strongly suggest that the wide variety in behaviour observed in NS-LXMBs with different luminosities can be linked through changes in a single variable parameter, namely the mass accretion rate, without the need for additional differences in the neutron star parameters or viewing angle. We briefly discuss the implications of our findings for the spectral changes observed in NS LMXBs and suggest that, contrary to what is often assumed, the position along the colour-colour tracks of Z sources is not determined by the instantaneous mass accretion rate.

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