Measuring glitch recoveries and braking indices with Bayesian model selection
arxiv(2024)
摘要
For a selection of 35 pulsars with large spin-up glitches
(Δν/ν≥10^-6), which are monitored by the Jodrell Bank
Observatory, we analyse 157 glitches and their recoveries. All parameters are
measured consistently and we choose the best model to describe the post-glitch
recovery based on Bayesian evidence. We present updated glitch epochs, sizes,
changes of spin down rate, exponentially recovering components (amplitude and
corresponding timescale) when present, as well as pulsars' second frequency
derivatives and their glitch associated changes if detected. We discuss the
different observed styles of post-glitch recovery as well as some particularly
interesting sources. Several correlations are revealed between glitch
parameters and pulsar spin parameters, including a very strong correlation
between a pulsar's interglitch |ν̈| and ν̇, as well as
between the glitch-induced spin-down rate change Δν̇_ p that
does not relax exponentially and ν̇. We find that the ratio
|Δν̇_p/ν̈| can be used as an
estimate of glitch recurrence times, especially for those pulsars for which
there are indications of a characteristic glitch size and interglitch waiting
time. We calculate the interglitch braking index n and find that pulsars with
large glitches typically have n greater than 3, suggesting that internal
torques dominate the rotational evolution between glitches. The external
torque, e.g. from electromagnetic dipole radiation, could dominate the observed
ν̈ for the youngest pulsars (≲10^4 yr), which
may be expected to display n∼3.
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