The evolution of PSR J0737−3039B and a model for relativistic spin precession

We present the evolution of the radio emission from the 2.8‐s pulsar of the double pulsar system PSR $\mathrm{J}\text{0737−3039}\mathrm{A/B}.$ We describe the changes in the pulse profile and flux density over five years of observations, culminating in the B pulsar’s radio disappearance in 2008 March. Over this time, the flux density decreased by $\text{0.177\hspace{0.17em}}\mathrm{mJy}\hspace{0.17em}{\mathrm{yr}}^{\text{−1}}$ at the brightest orbital phases and the pulse profile evolved from a single to a double peak. Relativistic spin precession, coupled with an elliptical beam, can model the pulse profile evolution well and the reappearance is expected to happen in ∼2035 with the same part of the beam or in ∼2014 if we assume a symmetric beam shape.