Fermion zero-mode influence on neutron-star magnetic field evolution

Jones, P. B.

doi:10.1111/j.1365-2966.2009.15016.x

Cited by 9 publications

(17 citation statements)

References 39 publications

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“…The frictional force on a flux tube due to scattering of zero modes localized inside the flux tube off gapless fermions in the bulk [44,45] has been calculated for proton flux tubes in nuclear matter [33]. At low temperatures, we expect the frictional force on a 2SC flux tube to be…”

Section: F Zero-mode Forcementioning

confidence: 99%

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Color-magnetic flux tubes in quark matter cores of neutron stars

Alford¹,

Sedrakian²

2010

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

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We argue that if color-superconducting quark matter exists in the core of a neutron star, it may contain a high density of flux tubes, carrying flux that is mostly color-magnetic, with a small admixture of ordinary magnetic flux. We focus on the two-flavor color-superconducting ("2SC") phase, and assume that the flux tubes are energetically stable, although this has not yet been demonstrated. The density of flux tubes depends on the nature of the transition to the colorsuperconducting phase, and could be within an order of magnitude of the density of magnetic flux tubes that would be found if the core were superconducting nuclear matter. We calculate the crosssection for Aharonov-Bohm scattering of gapless fermions off the flux tubes, and the associated collision time and frictional force on a moving flux tube. We discuss the other forces on the flux tube, and find that if we take in to account only the forces that arise within the 2SC core region then the timescale for expulsion of the color flux tubes from the 2SC core is of order 10 10 years.

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Section: F Zero-mode Forcementioning

confidence: 99%

“…(There is controversy about this in the literature; for example, Jones [33,43] has suggested that this is cancelled by another contribution from ungapped fermions. Pending a definitive resolution of this disagreement we will use the standard form of the Magnus-Lorentz force.…”

Section: Magnus-lorentz Forcementioning

confidence: 99%

Color-magnetic flux tubes in quark matter cores of neutron stars

Alford¹,

Sedrakian²

2010

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

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“…The existence of fermion degrees of freedom is also important at the macroscopic level, as pointed out by Jones 66 . As is known in superfluid and superconducting systems, fermion bound states in the vortex core seriously affect vortex dynamics through the spectral flow force [67][68][69] .…”

Section: Introductionmentioning

confidence: 97%

Microscopic description of axisymmetric vortices in P23 superfluids

Yumoto

Mizushima

Nitta

2020

Phys. Rev. Research

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We study quantized vortices in 3 P 2 superfluids using a microscopic theory for the first time. The theory is based on the Eilenberger equation to determine the order parameters and the Bogoliubov-de Gennes (BdG) equation to obtain the eigenenergies and the core magnetization. Within axisymmetric vortex configurations, we find several stable and metastable vortex configurations which depend on the strength of a magnetic field, similar to a v-vortex and o-vortex in 3 He superfluids. We demonstrate that the o-vortex is the most stable axisymmetric vortex in the presence of a strong magnetic field, and find two zero-energy Majorana fermion bound states in the o-vortex core. We show that the profiles of the core magnetization calculated using the BdG equation are drastically different from those calculated using only the order parameter profiles known before.

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“…Alternatively, such a braking index can be accounted for if the magnetic dipole braking still dominates but the star is experiencing a long-term dipole magnetic field decay. The surface dipole magnetic field has a significant effect on the spin evolution of a pulsar, as well as on its braking index (e.g., Goldreich & Reisenegger 1992;Tauris & Konar 2001;Jones 2009;Marchant et al 2014). In the case of a varying dipole magnetic field at the pole B p , the braking index n can be simply expressed as follows: Kaminker et al 2014;Potekhin et al 2015), whereas n 3 < for an increasing B p (e.g., Mereghetti 2008;Gao et al 2016).…”

Section: Introductionmentioning

confidence: 99%

The Dipole Magnetic Field and Spin-down Evolutions of the High Braking Index Pulsar PSR J1640–4631

Gao

Wang

Shan

et al. 2017

ApJ

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In this work, we interpreted the high braking index of PSR J1640−4631 with a combination of the magnetodipole radiation and dipole magnetic field decay models. By introducing a mean rotation energy conversion coefficient z , the ratio of the total high-energy photon energy to the total rotation energy loss in the whole life of the pulsar, and combining the pulsar's high-energy and timing observations with a reliable nuclear equation of state, we estimate the pulsar's initial spin period, P 17 44 0~( -) ms, corresponding to the moment of inertia I 0.8 2.1 10 45( -) g cm 2 .Assuming that PSR J1640−4631 has experienced a long-term exponential decay of the dipole magnetic field, we calculate the true age t age , the effective magnetic field decay timescale D t , and the initial surface dipole magnetic field at the pole B 0 p ( ) of the pulsar to be 2900−3100 yr, 1.07 2 10 5 ( ) yr, and 1.84 4.20 10 13 ( -) G, respectively. The measured braking index of n 3.15 3 = ( ) for PSR J1640−4631 is attributed to its long-term dipole magnetic field decay and a low magnetic field decay rate, dB dt 1.66 3.85 10 p 8-( -) G yr −1 . Our model can be applied to both the high braking index (n 3 > ) and low braking index (n 3 < ) pulsars, tested by the future polarization, timing, and high-energy observations of PSR J1640−4631.

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Fermion zero-mode influence on neutron-star magnetic field evolution

Cited by 9 publications

References 39 publications

Color-magnetic flux tubes in quark matter cores of neutron stars

Color-magnetic flux tubes in quark matter cores of neutron stars

Microscopic description of axisymmetric vortices in P23 superfluids

The Dipole Magnetic Field and Spin-down Evolutions of the High Braking Index Pulsar PSR J1640–4631

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