Crustal Entrainment and Pulsar Glitches

Chamel, Nicolas

doi:10.1103/physrevlett.110.011101

Cited by 219 publications

(280 citation statements)

References 53 publications

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“…More generally the forces that we calculate can be used to generate realistic pinning profiles for glitch models (Haskell, Pizzochero & Sidery 2013;Haskell & Antonopoulou 2013), simulations of vortex dynamics in neutron stars (Warszawski & Melatos 2008) or mode calculations (Glampedakis & Andersson 2009;Link 2012). Future work will aim to include consistently the effect of strong crustal entrainment, as Link (2014) has shown that including entrainment phenomenologically by rescaling the free neutron density can have important consequences for vortex creep, and more generally strong entrainment provides strong constraints for glitch models (Andersson et al 2012;Chamel 2013).…”

Section: Discussionmentioning

confidence: 99%

“…A more detailed study of the dependence of the snowplow model on parameters such as the equation of state and the mass of the star can be found in Seveso et al (2012) and Haskell, Pizzochero & Seveso (2013). Effects of superfluid entrainment will also be considered in future work, as strong entrainment in the crust can severely limit the amount of angular momentum that is exchanged during a glitch and allow to set constraints on the equation of state (Andersson et al 2012;Chamel 2013).…”

Section: Application To Pulsar Glitchesmentioning

confidence: 99%

“…This quantity obviously determines the maximum amount of angular momentum that can be exchanged during a glitch. An understanding of how much angular momentum can be stored in different regions of the star would, in fact, allow detailed comparisons with observations of glitching pulsars and potentially constrain the equation of state of dense matter (Andersson et al 2012;Chamel 2013;Piekarewickz, Fattoyev & Horowitz 2014).…”

Section: Introductionmentioning

confidence: 99%

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Mesoscopic pinning forces in neutron star crusts

Seveso¹,

Pizzochero²,

Grill³

et al. 2015

Mon. Not. R. Astron. Soc.

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The crust of a neutron star is thought to be comprised of a lattice of nuclei immersed in a sea of free electrons and neutrons. As the neutrons are superfluid their angular momentum is carried by an array of quantized vortices. These vortices can pin to the nuclear lattice and prevent the neutron superfluid from spinning down, allowing it to store angular momentum which can then be released catastrophically, giving rise to a pulsar glitch. A crucial ingredient for this model is the maximum pinning force that the lattice can exert on the vortices, as this allows us to estimate the angular momentum that can be exchanged during a glitch. In this paper we perform, for the first time, a detailed and quantitative calculation of the pinning force per unit length acting on a vortex immersed in the crust and resulting from the mesoscopic vortexlattice interaction. We consider realistic vortex tensions, allow for displacement of the nuclei and average over all possible orientation of the crystal with respect to the vortex. We find that, as expected, the mesoscopic pinning force becomes weaker for longer vortices and is generally much smaller than previous estimates, based on vortices aligned with the crystal. Nevertheless the forces we obtain still have maximum values of order f pin ≈ 10 15 dyn/cm, which would still allow for enough angular momentum to be stored in the crust to explain large Vela glitches, if part of the star is decoupled during the event.

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Section: Discussionmentioning

confidence: 99%

Section: Application To Pulsar Glitchesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Mesoscopic pinning forces in neutron star crusts

Seveso¹,

Pizzochero²,

Grill³

et al. 2015

Mon. Not. R. Astron. Soc.

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“…[51], the authors estimated that the observed glitches of Vela would be explained if 1.4% of the total momentum of inertia of the star resides in the crust. More recently, it was shown that crustal entrainment requires, in fact, a larger angular-momentum reservoir in the crust [52] associated with a fraction of the total momentum of inertia larger than that the crust may contain. Possible solutions to solve this problem include the contribution of the core to the glitch mechanism [53], or the choice of an appropriate EoS that predicts a sufficiently large pressure at the crust-core transition [54].…”

Section: Introductionmentioning

confidence: 99%

Vlasov formalism for extended relativistic mean field models: The crust-core transition and the stellar matter equation of state

Pais

Providência

2016

Phys. Rev. C

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The Vlasov formalism is extended to relativistic mean field hadron models with nonlinear terms up to fourth order and applied to the calculation of the crust-core transition density. The effect of the nonlinear ωρ and σρ coupling terms on the crust-core transition density and pressure and on the macroscopic properties of some families of hadronic stars is investigated. For that purpose, six families of relativistic mean field models are considered. Within each family, the members differ in the symmetry energy behavior. For all the models, the dynamical spinodals are calculated, and the crust-core transition density and pressure and the neutron star mass-radius relations are obtained. The effect on the star radius of the inclusion of a pasta calculation in the inner crust is discussed. The set of six models that best satisfy terrestrial and observational constraints predicts a radius of 13.6 ± 0.3 km and a crust thickness of 1.36 ± 0.06 km for a 1.4M star.

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“…However, recent calculations of the strength of the entrainment of superfluid neutrons by the crustal lattice via Bragg scattering suggest that only a fraction of the crustal neutrons are effectively free, and consequently the upper limit to the moment of inertia of the angular momentum reservoir is reduced: ∆I ∼ 0.2I csf . Initial analyses suggested that makes ∆I/I too small to explain the observed glitch sizes (Chamel 2013(Chamel , 2012Andersson et al 2012), and suggests one must at least involve other components of the star in addition to the crust superfluid as the store of angular momentum. These studies assume a strong coupling between crust and core so that I ∼ Itot.…”

Section: Introductionmentioning

confidence: 99%

Efficacy of crustal superfluid neutrons in pulsar glitch models

Hooker¹,

Newton²,

Li³

2015

Monthly Notices of the Royal Astronomical Society

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In order to assess the ability of purely crust-driven glitch models to match the observed glitch activity in the Vela pulsar, we conduct a systematic analysis of the dependence of the fractional moment of inertia of the inner crustal neutrons on the stiffness of the nuclear symmetry energy at saturation density L. We take into account both crustal entrainment and the fact that only a fraction Y g of the core neutrons may couple to the crust on the glitch-rise timescale. We use a set of consistently-generated crust and core compositions and equations-of-state which are fit to results of lowdensity pure neutron matter calculations. When entrainment is included at the level suggested by recent microscopic calculations and the core is fully coupled to the crust, the model is only able to account for the Vela glitch activity for a 1.4M star if the equation of state is particularly stiff L > 100 MeV. However, an uncertainty of about 10% in the crust-core transition density and pressure allows for the Vela glitch activity to be marginally accounted for in the range L ≈ 30 − 60MeV consistent with a range of experimental results. Alternatively, only a small amount of core neutrons need be involved. If less than 50% of the core neutrons are coupled to the crust during the glitch, we can also account for the Vela glitch activity using crustal neutrons alone for EOSs consistent with the inferred range of L. We also explore the possibility of Vela being a high-mass neutron star, and of crustal entrainment being reduced or enhanced relative to its currently predicted values.

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Crustal Entrainment and Pulsar Glitches

Cited by 219 publications

References 53 publications

Mesoscopic pinning forces in neutron star crusts

Mesoscopic pinning forces in neutron star crusts

Vlasov formalism for extended relativistic mean field models: The crust-core transition and the stellar matter equation of state

Efficacy of crustal superfluid neutrons in pulsar glitch models

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