On the magnetic field evolution time-scale in superconducting neutron star cores

Passamonti, Andrea; Akgün, Taner; Pons, José A.; Miralles, J. A.

doi:10.1093/mnras/stx1192

Cited by 34 publications

(41 citation statements)

References 29 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Core-field evolution is a much more vexed issue, mainly due to the uncertain role played by superfluid components (which are present even in magnetars younger than any observed to date; Ho et al (2012)). There are debates about whether any core process is fast enough to be relevant to magnetars; providing arbitration of the dispute is beyond the scope of this paper, but for a flavour of the recent literature see, e.g., Jones (2006); Glampedakis et al (2011b); Graber et al (2015); Gügercinoglu & Alpar (2016); Dommes & Gusakov (2017); Passamonti et al (2017); Castillo et al (2017); Ofengeim & Gusakov (2018). There is also little understanding about how core and crust are linked, and the physics at the boundary that separates them.…”

Section: Introductionmentioning

confidence: 99%

Magnetic-field evolution in a plastically failing neutron-star crust

Lander

Gourgouliatos

2019

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Under normal conditions in a neutron-star crust, ions are locked in place in the crustal lattice and only electrons are mobile, and magnetic-field evolution is thus directly related to the electron velocity. The evolution, however, builds magnetic stresses that can become sufficiently large for the crust to exceed its elastic limit, and to flow plastically. We consider the nature of this plastic flow and the back-reaction on the crustal magnetic field evolution. We formulate a plane-parallel model for the local failure, showing that surface motions are inevitable once the crust yields, in the absence of extra dissipative mechanisms. We perform numerical evolutions of the crustal magnetic field under the joint effect of Hall drift and Ohmic decay, tracking the build-up of magnetic stresses, and diagnosing crustal failure with the von Mises criterion. Beyond this point we solve for the coupled evolution of the plastic velocity and magnetic field. Our results suggest that to have a coexistence of a magnetar corona with small-scale magnetic features, the viscosity of the plastic flow must be roughly 10 36 − 10 37 g cm −1 s −1 . We find significant motion at the surface at a rate of 10 − 100 centimetres per year, and that the localised magnetic field is weaker than in evolutions without plastic flow. We discuss astrophysical implications, and how our local simulations could be used to build a global model of field evolution in the neutron-star crust.

show abstract

Section: Introductionmentioning

confidence: 99%

Magnetic-field evolution in a plastically failing neutron-star crust

Lander

Gourgouliatos

2019

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…Other recent works (Graber et al 2015;Elfritz et al 2016) have also shown that, without considering ambipolar diffusion, the magnetic flux expulsion from the NS core with superconducting protons is very slow. In Passamonti et al (2017a) the various approximations employed to study the long-term evolution of the magnetic field in NS cores were revisited, solving a recent controversy (Graber et al 2015;Dommes and Gusakov 2017) on the correct form of the induction equation and the relevant evolution timescale in superconducting NS cores.…”

Section: Ambipolar Diffusion In Neutron Star Coresmentioning

confidence: 99%

Magnetic, thermal and rotational evolution of isolated neutron stars

Pons

Viganò

2019

Living Rev Comput Astrophys

Self Cite

106

View full text Add to dashboard Cite

The strong magnetic field of neutron stars is intimately coupled to the observed temperature and spectral properties, as well as to the observed timing properties (distribution of spin periods and period derivatives). Thus, a proper theoretical and numerical study of the magnetic field evolution equations, supplemented with detailed calculations of microphysical properties (heat and electrical conductivity, neutrino emission rates) is crucial to understand how the strength and topology of the magnetic field vary as a function of age, which in turn is the key to decipher the physical processes behind the varied neutron star phenomenology. In this review, we go through the basic theory describing the magneto-thermal evolution models of neutron stars, focusing on numerical techniques, and providing a battery of benchmark tests to be used as a reference for present and future code developments. We summarize well-known results from axisymmetric cases, give a new look at the latest 3D advances, and present an overview of the expectations for the field in the coming years.

show abstract

“…The magnetic dynamics of the Type II superconductor in coupling with the rotational dynamics of the neutron superfluid is a complicated problem for which the detailed solution on all different timescales is not known (Passamonti et al 2017). The essentials relevant for the evolutionary scenario of Srinivasan et al (1990) were presented in an important paper by Ruderman et al (1998).…”

Section: Flux-vortex Pinningmentioning

confidence: 99%

“…The rotational (solenoidal) electric field E = −1/c(∂A/∂t) which plays the leading role in the dynamics of magnetic field decay (Passamonti et al 2017) is set up by the radial flow of flux lines in the case of a Type II superconductor:…”

Section: Flux-vortex Pinningmentioning

confidence: 99%

Flux-Vortex Pinning and Neutron Star Evolution

Alpar

2017

J Astrophys Astron

View full text Add to dashboard Cite

Abstract. G. Srinivasan et al. (1990) proposed a simple and elegant explanation for the reduction of the neutron star magnetic dipole moment during binary evolution leading to low mass X-ray binaries and eventually to millisecond pulsars: Quantized vortex lines in the neutron star core superfluid will pin against the quantized flux lines of the proton superconductor. As the neutron star spins down in the wind accretion phase of binary evolution, outward motion of vortex lines will reduce the dipole magnetic moment in proportion to the rotation rate. The presence of a toroidal array of flux lines makes this mechanism inevitable and independent of the angle between the rotation and magnetic axes. The incompressibility of the flux-line array (Abrikosov lattice) determines the epoch when the mechanism will be effective throughout the neutron star. Flux vortex pinning will not be effective during the initial young radio pulsar phase. It will, however, be effective and reduce the dipole moment in proportion with the rotation rate during the epoch of spindown by wind accretion as proposed by Srinivasan et al. The mechanism operates also in the presence of vortex creep.

show abstract

On the magnetic field evolution time-scale in superconducting neutron star cores

Cited by 34 publications

References 29 publications

Magnetic-field evolution in a plastically failing neutron-star crust

Magnetic-field evolution in a plastically failing neutron-star crust

Magnetic, thermal and rotational evolution of isolated neutron stars

Flux-Vortex Pinning and Neutron Star Evolution

Contact Info

Product

Resources

About