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We investigate rotational spin noise (referred to as timing noise) innon-accreting pulsars: millisecond pulsars, canonical pulsars, and magnetars.Particular attention is placed on quantifying the strength and non-stationarityof timing noise in millisecond pulsars because the long-term stability of theseobjects is required to detect nanohertz gravitational radiation. We show that asingle scaling law is sufficient to characterize timing noise in millisecondand canonical pulsars while the same scaling law underestimates the levels oftiming noise in magnetars. The scaling law, along with a detailed study of themillisecond pulsar B1937+21, leads us to conclude that timing noise is latentin most millisecond pulsars and will be measurable in many objects when betterarrival time estimates are obtained over long data spans. The sensitivity of apulsar timing array to gravitational radiation is strongly affected by anytiming noise. We conclude that detection of proposed gravitational wavebackgrounds will require the analysis of more objects than previously suggestedover data spans that depend on the spectra of both the gravitational wavebackground and of the timing noise. It is imperative to find additionalmillisecond pulsars in current and future surveys in order to reduce theeffects of timing noise.

Assessing the Role of Spin Noise in the Precision Timing of Millisecond Pulsars