The Evolution of the High Energy Tail in the Quiescent Spectrum of the Soft

A moderate level of variability has been detected in the quiescent luminosity of several neutron star soft X– ray transients. Spectral variability was first revealed by Chandra observations of Aql X-1 in the four months that followed the 2000 X–ray outburst. By adopting the canonical model for quiescent spectrum of soft X–ray transients, i.e. an absorbed neutron star atmosphere model plus a power law tail, Rutledge et al. (2002a) concluded that the observed spectral variations can be ascribed to temperature variations of the neutron star atmosphere. These results can hardly be reconciled with the neutron star cooling that is expected to take place in between outbursts (after deep crustal heating in the accretion phase). Here we reanalyse the Chandra spectra of Aql X-1, together with a long BeppoSAX observation in the same period, and propose a different interpretation of the spectral variability: that this is due to correlated variations of the power law component and the column density (> 5, a part of which might be intrinsic to the source), while the temperature and flux of the neutron star atmospheric component remained unchanged. This lends support to the idea that the power law component arises from emission at the shock between a radio pulsar wind and inflowing matter from the companion star. Subject headings: accretion, accretion disks — binaries: close — star: individual (Aql X-1) — stars: neutron