Pulsar Glitch in a Strangeon Star Model. III. The recovery

Abstract

Strangeon star model has passed various observational tests, such as the massive pulsars and the tidal deformability during binary mergers. Pulsar glitch, as a useful probe for studying the interior structure of pulsars, has also been studied in strangeon star model in our previous papers, including the recovery coefficient, the waiting time of glitches and glitch activity. In this paper, the recovery process of a glitch is described in the strangeon star model, based on the starquake picture established in Paper I. After the starquake, the inner motion of the stellar matter would reduce the tangential pressure in the cracked places at the equatorial plane. The recovery (increase) of the tangential pressure would be achieved by a viscous flow towards the cracked places at equatorial plane, which leads to the exponential recovery of the spin frequency. A uniform viscous flow can reproduce the single exponential decay observed in some glitches, and the viscous time-scale $\tau$ and the depth $h$ of the cracking place below the surface can be fitted by the recovery data. It is found that $h$ increases with glitch size $\Delta \nu /\nu$, which is expected in the glitch scenario of strangeon stars. The magnitude of the recovery predicted in this recovery model is also consistent with that derived from observations. The single exponential decay reproduced by a uniform viscous flow can be generalized to two or more exponentials by the multi-component of viscous flows.

7 pages, 4 figures, 1 table. Accepted for publication in MNRAS

References in corpus (20)

• GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral
• Shapiro delay measurement of a two solar mass neutron star
• Color superconductivity in dense quark matter
• Origin of the heavy elements in binary neutron-star mergers from a gravitational wave event
• Illuminating Gravitational Waves: A Concordant Picture of Photons from a Neutron Star Merger
• Infrared Properties of QCD from Dyson-Schwinger equations
• Re-detection and a Possible Time Variation of Soft X-ray Polarisation from the Crab
• Searches for Gravitational Waves from Known Pulsars at Two Harmonics in the Second and Third LIGO-Virgo Observing Runs
• A Polytropic Model of Quark Stars
• The superflares of soft Gamma-ray repeatres: giant quakes in solid quark stars?
• Two types of glitches in a solid quark star model
• A Cellular Automaton Model of Pulsar Glitches
• Superfluid vortex unpinning as a coherent noise process, and the scale invariance of pulsar glitches
• Pulsar slow glitches in a solid quark star model
• Results of 12 Years of Pulsar Timing at Nanshan -- I
• Pulsar glitches in a strangeon star model. II. The activity
• Bulk Strong Matter: the Trinity
• Merging strangeon stars II: the ejecta and light curves
• Quakes of Compact Stars
• The precursor of GRB211211A: a tide-induced giant quake?

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• Strange Matter
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