Kolmogorov analysis of pulsar TOA | Astronomy & Astrophysics (A&A)

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Fig. 5.

KSP distributions for the pulsar J1022+1001 after introducing the time dependence in β. Although ⟨χ²⟩ is smaller in the β(t) approach (Table 2) than in the β = const case (Table 1), they are of the same order.

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