A simple mechanism for the anti-glitch observed in AXP 1E 2259+586

García, Federico; Ranea‐Sandoval, Ignacio F.

doi:10.1093/mnrasl/slv019

Cited by 15 publications

(42 citation statements)

References 36 publications

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“…We hold Bp = 5.3 × 10 13 G constant, corresponding to the value inferred from spin down, and allow Bt to change. Figure 1 shows that the toroidal field strength must decrease from its initial value to give an anti-glitch of the observed magnitude, as noted by García & Ranea-Sandoval (2015), with each curve approaching a particular value of B i t as B f t → 0. This minimum allowed value for B i t is found by setting ǫ f = ǫmax in equation (10), where the maximum ellipticity ǫmax is obtained by setting Λ = 1 (a purely poloidal configuration) in equation (9).…”

Section: Axp 1e 2259+586 Anti-glitchmentioning

confidence: 80%

“…Some critical strain is then reached, when the crust cracks in a sudden event (i.e., the outburst), and the star settles into a new field configuration with ǫ f > ǫi. The change in frequency (i.e., the anti-glitch) arises from a change in moment of inertia (because angular momentum is conserved), which is then related to the change in ǫ to give equation (4) in García & Ranea-Sandoval (2015), reproduced here as equation (10). The measured frequency change associated with the anti-glitch is −5 × 10 −7 Hz over ∼ 10 2 d (Archibald et al 2013).…”

Section: Axp 1e 2259+586 Anti-glitchmentioning

confidence: 99%

“…For example, in order for a star with M * = 1.4 M⊙ and R * = 10 4 m [solid curves in Fig. 1 in this paper and in García & Ranea-Sandoval (2015)] to give ∆ν/ν = −6.3×10 −7 , the toroidal field must decrease from…”

Section: Axp 1e 2259+586 Anti-glitchmentioning

confidence: 99%

“…We investigate a range of initial and final states, that give the observed anti-glitch magnitude, comparing our results directly to those of García & Ranea-Sandoval (2015). In Section 3, we construct a dipole-plus-quadrupole twisted torus, apply it to AXP 1E 2259+586, and repeat the test over a range of initial and final states.…”

mentioning

confidence: 99%

“…In Section 4, we calculate the energy released during these changes in field configuration and compare them to the observed outburst energy. We keep the dipole poloidal field strength Bp = 5.9 × 10 13 G constant throughout this paper, corresponding to the spin-down-inferred value, as García & Ranea-Sandoval (2015) did. In other words, like they did, we assume that the frequency change is purely due to a decay of the internal toroidal field (Section 2) or the quadrupole component (Section 3), and the dipole poloidal field (which is responsible for overall spin down) remains unchanged before and after the glitch (García & Ranea-Sandoval 2015).…”

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confidence: 99%

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Interpreting the AXP 1E 2259+586 antiglitch as a change in internal magnetization

Mastrano

Suvorov

Melatos

2015

Mon. Not. R. Astron. Soc.

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The sudden spin-down event ('anti-glitch') observed in AXP 1E 2259+586 on 2012 April 21 was arguably caused by a decay of its internal toroidal magnetic field component, which turns a stable prolate configuration into an unstable one. We refine previous models of this process by modelling the star's magnetic field self-consistently as a 'twisted torus' configuration in non-barotropic equilibrium (which allows us to explore a greater range of equilibrium configurations). It is shown that, if the star's magnetic field is purely dipolar, the change in the toroidal field strength required to produce an anti-glitch of the observed size can be ∼ 10 times larger than previously calculated. If the star has a quadrupolar magnetic field component, then an anti-glitch of similar magnitude can be produced via a decay of the quadrupole component, in addition to a decay of the toroidal component. We show that, if the quadrupole component decays, the minimum initial toroidal field strength and the change in toroidal field strength needed to produce the observed anti-glitch are lower than in the pure dipole twisted torus. In addition, we predict the maximum anti-glitch sizes, assuming that they are caused by a change in ellipticity, in four glitching magnetars and discuss the implications for energetics of accompanying X-ray bursts.

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Section: Axp 1e 2259+586 Anti-glitchmentioning

confidence: 80%

Section: Axp 1e 2259+586 Anti-glitchmentioning

confidence: 99%

Section: Axp 1e 2259+586 Anti-glitchmentioning

confidence: 99%

mentioning

confidence: 99%

mentioning

confidence: 99%

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Interpreting the AXP 1E 2259+586 antiglitch as a change in internal magnetization

Mastrano

Suvorov

Melatos

2015

Mon. Not. R. Astron. Soc.

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Phase transitions in neutron stars and their links to gravitational waves

Orsaria

Malfatti

Mariani

et al. 2019

J. Phys. G: Nucl. Part. Phys.

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The recent direct observation of gravitational wave event GW 170817 and its GRB170817A signal has opened up a new window to study neutron stars and heralds a new era of Astronomy referred to as the Multimessenger Astronomy. Both gravitational and electromagnetic waves from a single astrophysical source have been detected for the first time. This combined detection offers an unprecedented opportunity to place constraints on the neutron star matter equation of state. The existence of a possible hadron-quark phase transition in the central regions of neutron stars is associated with the appearance of g-modes, which are extremely important as they could signal the presence of a pure quark matter core in the centers of neutron stars. Observations of g-modes with frequencies between 1 kHz and 1.5 kHz could be interpreted as evidence of a sharp hadron-quark phase transition in the cores of neutron stars. In this article, we shall review the description of the dense matter composing neutron stars, the determination of the equation of state of such matter, and the constraints imposed by astrophysical observations of these fascinating compact objects. arXiv:1907.04654v1 [astro-ph.HE]

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Pulsar glitches: observations and physical interpretation

Antonopoulou¹,

Haskell²,

Espinoza³

2022

Rep. Prog. Phys.

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The interpretation of pulsar rotational glitches, the sudden increase in spin frequency of neutron stars, is a half-century-old challenge. The common view is that glitches are driven by the dynamics of the stellar interior, and connect in particular to the interactions between a large-scale neutron superfluid and the other stellar components. This thesis is corroborated by observational data of glitches and the post-glitch response seen in pulsars' rotation, which often involves very long timescales, from months to years. As such, glitch observables combined with consistent models incorporating the rich physics of neutron stars -- from the lattice structure of their crust to the equation of state for matter beyond nuclear densities -- can be very powerful at placing limits on, and reduce uncertainties of, the internal properties. This review summarises glitch observations, current data, and recent analyses, and connects them to the underlying mechanisms and microphysical parameters in the context of the most advanced theoretical glitch models to date.

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A simple mechanism for the anti-glitch observed in AXP 1E 2259+586

Cited by 15 publications

References 36 publications

Interpreting the AXP 1E 2259+586 antiglitch as a change in internal magnetization

Interpreting the AXP 1E 2259+586 antiglitch as a change in internal magnetization

Phase transitions in neutron stars and their links to gravitational waves

Pulsar glitches: observations and physical interpretation

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