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The primary goal of the pulsar timing array projects is to detectultra-low-frequency gravitational waves. The pulsar data sets are affected bynumerous noise processes including varying dispersive delays in theinterstellar medium and from the solar wind. The solar wind can lead to rapidlychanging variations that, with existing telescopes, can be hard to measure andthen remove. In this paper we study the possibility of using a low frequencytelescope to aid in such correction for the Parkes Pulsar Timing Array (PPTA)and also discuss whether the ultra-wide-bandwidth receiver for the FASTtelescope is sufficient to model the solar wind variations. Our key result isthat a single wide-bandwidth receiver can be used to model and remove theeffect of the solar wind. However, for pulsars that pass close to the Sun suchas PSR J1022+1022, the solar wind is so variable that observations at twotelescopes separated by a day are insufficient to correct the solar windeffect.

Correcting for the solar wind in pulsar timing observations: the role of simultaneous a nd l ow-frequency observations