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We present the evolution of the radio emission from the 2.8-s pulsar of thedouble pulsar system PSR J0737-3039A/B. We provide an update on the Burgay etal. (2005) analysis by describing the changes in the pulse profile and fluxdensity over five years of observations, culminating in the B pulsar's radiodisappearance in 2008 March. Over this time, the flux density decreases by0.177 mJy/yr at the brightest orbital phases and the pulse profile evolves froma single to a double peak, with a separation rate of 2.6 deg/yr. The pulseprofile changes are most likely caused by relativistic spin precession, but cannot be easily explained with a circular hollow-cone beam as in the model ofClifton & Weisberg (2008). Relativistic spin precession, coupled with anelliptical beam, can model the pulse profile evolution well. This particularbeam shape predicts geometrical parameters for the two bright orbital phaseswhich are consistent and similar to those derived by Breton et al. (2008).However, the observed decrease in flux over time and B's eventual disappearancecannot be easily explained by the model and may be due to the changinginfluence of A on B.

The Evolution of PSR J0737-3039B and a Model for Relativistic Spin Precession