Magnetic Fields in Superconducting Neutron Stars

Lander, S. K.

doi:10.1103/physrevlett.110.071101

Cited by 73 publications

(68 citation statements)

References 39 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The equilibrium magnetic structure and its stability are then controlled by H c1 / B at the crust-core boundary Lander 2013Lander , 2014. In fact, the internal field configuration now depends very strongly on field strength, suggesting significant differences between the interior fields of pulsars and those of magnetars (Lander 2014).…”

Section: Generation Physicsmentioning

confidence: 99%

Magnetic Field Generation in Stars

2015

View full text Add to dashboard Cite

Enormous progress has been made on observing stellar magnetism in stars from the main sequence through to compact objects. Recent data have thrown into sharper relief the vexed question of the origin of stellar magnetic fields, which remains one of the main unanswered questions in astrophysics. In this chapter we review recent work in this area of research. In particular, we look at the fossil field hypothesis which links magnetism in compact stars to magnetism in main sequence and pre-main sequence stars and we consider why its feasibility has now been questioned particularly in the context of highly magnetic white dwarfs. We also review the fossil versus dynamo debate in the context of neutron stars and the roles played by key physical processes such as buoyancy, helicity, and superfluid turbulence,in the generation and stability of neutron star fields. Independent information on the internal magnetic field of neutron stars will come from future gravitational wave detections. Thus we maybe at the dawn of a new era of exciting discoveries in compact star magnetism driven by the opening of a new, non-electromagnetic observational window. We also review recent advances in the theory and computation of magnetohydrodynamic turbulence as it applies to stellar magnetism and dynamo theory. These advances offer insight into the action of stellar dynamos as well as processes whichcontrol the diffusive magnetic flux transport in stars.Comment: 41 pages, 7 figures. Invited review chapter on on magnetic field generation in stars to appear in Space Science Reviews, Springe

show abstract

Section: Generation Physicsmentioning

confidence: 99%

Magnetic Field Generation in Stars

2015

View full text Add to dashboard Cite

show abstract

“…In practice, this leads to larger distortions for the same B surf , compared with those obtained from a non-superconducting model like equation (15). The ellipticity relation now takes the form (Lander 2013(Lander , 2014:…”

Section: Ns Free Precessionmentioning

confidence: 99%

M51 ULX-7: superorbital periodicity and constraints on the neutron star magnetic field

Vasilopoulos

Lander

Koliopanos

et al. 2019

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

In the current work we explore the applicability of standard theoretical models of accretion to the observed properties of M51 ULX-7. The spin-up rate and observed X-ray luminosity are evidence of a neutron star with a surface magnetic field of 2 − 7 × 10 13 G, rotating near equilibrium. Analysis of the X-ray light-curve of the system (Swift/XRT data) reveals the presence of a ∼39 d super-orbital period. We argue that the super-orbital periodicity is due to disc precession, and that material is accreted onto the neutron star at a constant rate throughout it. Moreover, by attributing this modulation to the free precession of the neutron star we estimate a surface magnetic field strength of 3 − 4 × 10 13 G. The agreement of these two independent estimates provide strong constraints on the surface polar magnetic field strength of the neutron star.

show abstract

“…Such current sheets are more prominent on the natural boundaries of the crust-core interface (Lander 2013;) and neutron star surface (Thompson & Duncan 2001;Lyubarsky et al 2002), providing potential sites for the tearing instability.…”

Section: Neutron Star Crust Heating and Outburstsmentioning

confidence: 99%

Resistive tearing instability in electron MHD: application to neutron star crusts

Gourgouliatos¹,

Hollerbach²

2016

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

We study a resistive tearing instability developing in a system evolving through the combined effect of Hall drift in the Electron-MHD limit and Ohmic dissipation. We explore first the exponential growth of the instability in the linear case and we find the fastest growing mode, the corresponding eigenvalues and dispersion relation. The instability growth rate scales as γ ∝ B 2/3 σ −1/3 where B is the magnetic field and σ the electrical conductivity. We confirm the development of the tearing resistive instability in the fully non-linear case, in a plane parallel configuration where the magnetic field polarity reverses, through simulations of systems initiating in Hall equilibrium with some superimposed perturbation. Following a transient phase, during which there is some minor rearrangement of the magnetic field, the perturbation grows exponentially. Once the instability is fully developed the magnetic field forms the characteristic islands and X-type reconnection points, where Ohmic decay is enhanced. We discuss the implications of this instability for the local magnetic field evolution in neutron stars' crusts, proposing that it can contribute to heating near the surface of the star, as suggested by models of magnetar post-burst cooling. In particular, we find that a current sheet a few meters thick, covering as little as 1% of the total surface can provide 10 42 erg in thermal energy within a few days. We briefly discuss applications of this instability in other systems where the Hall effect operates such as protoplanetary discs and space plasmas.

show abstract

Magnetic Fields in Superconducting Neutron Stars

Cited by 73 publications

References 39 publications

Magnetic Field Generation in Stars

Magnetic Field Generation in Stars

M51 ULX-7: superorbital periodicity and constraints on the neutron star magnetic field

Resistive tearing instability in electron MHD: application to neutron star crusts

Contact Info

Product

Resources

About