Rotational evolution of the Vela pulsar during the 2016 glitch. (arXiv:1907.01124v1 [astro-ph.HE])

Rotational evolution of the Vela pulsar during the 2016 glitch. (arXiv:1907.01124v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Ashton_G/0/1/0/all/0/1">Gregory Ashton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lasky_P/0/1/0/all/0/1">Paul D. Lasky</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Graber_V/0/1/0/all/0/1">Vanessa Graber</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Palfreyman_J/0/1/0/all/0/1">Jim Palfreyman</a>

The 2016 Vela glitch observed by the Mt Pleasant radio telescope provides the
first opportunity to study pulse-to-pulse dynamics of a pulsar glitch, opening
up new possibilities to study the neutron star’s interior. We fit models of the
star’s rotation frequency to the pulsar data, and present three new results.
First, we constrain the glitch rise time to less than 12.6s with 90%
confidence, almost three times shorter than the previous best constraint.
Second, we find definitive evidence for a rotational-frequency overshoot and
fast relaxation following the glitch. Third, we find evidence for a slow-down
of the star’s rotation immediately prior to the glitch. The overshoot is
predicted theoretically by some models; we discuss implications of the glitch
rise and overshoot decay times on internal neutron-star physics. The slow down
preceding the glitch is unexpected; we propose the slow-down may trigger the
glitch by causing a critical lag between crustal superfluid and the crust.

The 2016 Vela glitch observed by the Mt Pleasant radio telescope provides the
first opportunity to study pulse-to-pulse dynamics of a pulsar glitch, opening
up new possibilities to study the neutron star’s interior. We fit models of the
star’s rotation frequency to the pulsar data, and present three new results.
First, we constrain the glitch rise time to less than 12.6s with 90%
confidence, almost three times shorter than the previous best constraint.
Second, we find definitive evidence for a rotational-frequency overshoot and
fast relaxation following the glitch. Third, we find evidence for a slow-down
of the star’s rotation immediately prior to the glitch. The overshoot is
predicted theoretically by some models; we discuss implications of the glitch
rise and overshoot decay times on internal neutron-star physics. The slow down
preceding the glitch is unexpected; we propose the slow-down may trigger the
glitch by causing a critical lag between crustal superfluid and the crust.

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