Vortices and type-I superconductivity in neutron stars

Buckley, K.; Metlitski, Max A.; Zhitnitsky, Ariel R.

doi:10.1103/physrevc.69.055803

Cited by 34 publications

(22 citation statements)

References 23 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…We have also verified [9] the above results numerically by solving the equations of motions corresponding to (1) with a particular choice of the approximately U(2) symmetric interaction potential V. Our numerical results support the analytical calculations given above. Namely, we find that the magnitude of the neutron condensate is slightly increased in the vortex core, the radius of the magnetic flux tube is of order , and the radius of the proton vortex core is of order = p .…”

supporting

confidence: 82%

Neutron Stars as Type-I Superconductors

2004

Self Cite

View full text Add to dashboard Cite

In a recent paper by Link, it was pointed out that the standard picture of the neutron star core composed of a mixture of a neutron superfluid and a proton type-II superconductor is inconsistent with observations of a long period precession in isolated pulsars. In the following we will show that an appropriate treatment of the interacting two-component superfluid (made of neutron and proton Cooper pairs), when the structure of proton vortices is strongly modified, may dramatically change the standard picture, resulting in a type-I superconductor. In this case the magnetic field is expelled from the superconducting regions of the neutron star, leading to the formation of the intermediate state when alternating domains of superconducting matter and normal matter coexist.

show abstract

supporting

confidence: 82%

Neutron Stars as Type-I Superconductors

2004

Self Cite

View full text Add to dashboard Cite

show abstract

“…The number density of such vortices is n v = B/Φ 0 ≈ 10 19 B 12 cm −2 , where B 12 = B/10 12 G. The knowledge of the electromagnetic properties of flux vortices in gravitational field may be relevant for understanding some observable phenomena of pulsars 9 . However, we should mention here that in recent papers (see, for example, 8 ) it was discussed inconsistency of the standard picture of the neutron star core, composed of a mixture of a neutron superfluid and a proton type-II superconductor with observations of long period precession in isolated pulsars.…”

Section: Introductionmentioning

confidence: 93%

Electromagnetic Effects in Superconductors in Stationary Gravitational Field

Ahmedov

Kagramanova

2005

Int. J. Mod. Phys. D

View full text Add to dashboard Cite

The general relativistic modifications to the resistive state in superconductors of second type in the presence of a stationary gravitational field are studied. Some superconducting devices that can measure the gravitational field by its red-shift effect on the frequency of radiation are suggested. It has been shown that by varying the orientation of a superconductor with respect to the earth gravitational field, a corresponding varying contribution to AC Josephson frequency would be added by gravity. A magnetic flux (being proportional to angular velocity of rotation Ω) through a rotating hollow superconducting cylinder with the radial gradient of temperature ∇rT is theoretically predicted. The magnetic flux is assumed to be produced by the azimuthal current arising from Coriolis force effect on radial thermoelectric current. Finally the magnetic flux through the superconducting ring with radial heat flow located at the equatorial plane interior the rotating neutron star is calculated. In particular it has been shown that nonvanishing magnetic flux will be generated due to the general relativistic effect of dragging of inertial frames on the thermoelectric current.

show abstract

“…In addition, the rotation of the neutron star causes a lattice of quantized vortices to form in the superfluid neutron state, similar to the observed vortices that form when superfluid Helium is rotated. However, according to recent work [27], a detailed analysis of both the proton and neutron Cooper pair condensates, indicates that the superconductor may in fact be type I with critical temperature H c ∼ 10 14 G and would exhibit the Meissner effect. This is in agreement with astrophysically based arguments indicating that the conventional picture of a neutron star as a type-II superconductor may have to be reconsidered [28].…”

Section: Superfluidity and Superconductivitymentioning

confidence: 99%

Magnetic Fields in High-Density Stellar Matter

Lugones¹

2005

AIP Conference Proceedings

View full text Add to dashboard Cite

Abstract. I briefly review some aspects of the effect of magnetic fields in the high density regime relevant to neutron stars, focusing mainly on compact star structure and composition, superconductivity, combustion processes, and gamma ray bursts. THE "MAGNETIC FIELD" OF "NEUTRON STARS"A large body of evidence now identifies the presence of strong magnetic fields at (or very near) the surface of neutron stars. Except for a few cases, all the estimations of the magnetic fields of these objects come from the timing measurements of pulsar slowdown. The pulsar is usually modelled as a rapidly rotating neutron star with a dipolar magnetic field configuration in which the rotation axis is not aligned with the dipole axis. Since the period of the pulsed emission is associated with the rotation period P, accurate observations of P and its time derivativesṖ,P, and even the third derivative of P, have been used to shed light on pulsar dynamics. Within this framework the dynamic equation readsΩ = KΩ 3 , with K ≡ (R 6 B 2 p sin 2 α)/(6c 3 I), and Ω = 2π/P. Therefore, some properties of pulsars are plausible of interpretation in terms of timing data, e.g.:• the component of the B-field at the magnetic pole along the rotation axis(1)• the pulsar age t (or alternatively the rotational period at birth P i ),where τ ≡ −P/2Ṗ is the so called characteristic age, I is the moment of inertia of the neutron star, R its radius, and α is the angle between the rotation axis and the dipole axis. Note that, for determining B ⊥ the values of I and R must be assumed based mostly on theoretical arguments. A test of the reliability of these estimates, can be obtained from an independent determination of the age of the pulsar, which is possible for pulsars associated with supernova remnants (SNRs). Assuming that a given pulsar and a given SNR were born together, we can identify t SNR (the SNR age) with the pulsar age t in Eq. (2). Since within the dipole model τ is an upper limit for t, a comparison of t SNR with τ provides a relevant

show abstract

Vortices and type-I superconductivity in neutron stars

Cited by 34 publications

References 23 publications

Neutron Stars as Type-I Superconductors

Neutron Stars as Type-I Superconductors

Electromagnetic Effects in Superconductors in Stationary Gravitational Field

Magnetic Fields in High-Density Stellar Matter

Contact Info

Product

Resources

About