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The outbursts of low mass X-ray binaries are prolonged relative to those ofdwarf nova cataclysmic variables as a consequence of X-ray irradiation of thedisc. We show that the time-scale of the decay light curve and its luminosityat a characteristic time are linked to the radius of the accretion disc. Hencea good X-ray light curve permits two independent estimates of the disc radius.In the case of the millisecond pulsars SAX J1808.4-3658 and XTE J0929-314 theagreement between these estimates is very strong. Our analysis allows newdeterminations of distances and accretion disc radii. Our analysis will allowdetermination of accretion disc radii for sources in external galaxies, andhence constrain system parameters where other observational techniques are notpossible. We also use the X-ray light curves to estimate the mass transferrate. The broken exponential decay observed in the 2002 outburst of SAXJ1808.4-3658 may be caused by the changing self-shadowing of the disc.

Modelling the outburst profile of X-ray powered millisecond pulsars