Magnetic field decay in isolated neutron stars
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Citations
Neutron Stars, Pulsars, and Pulsar Wind Nebulae
Gravitational-wave spin-down and stalling lower limits on the electrical resistivity of the accreted mountain in a millisecond pulsar
Shell model of magnetic field evolution under the hall effect
A deep XMM-Newton look on the thermally emitting isolated neutron star RX J1605.3+3249
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Formation of very strongly magnetized neutron stars - Implications for gamma-ray bursts
The soft gamma repeaters as very strongly magnetized neutron stars - I. Radiative mechanism for outbursts
Frequently Asked Questions (16)
Q2. What is the effect of the pressure gradients on nc v?
Since the weak interactions that restore chemical equilibrium are very sluggish at low temperatures, 5 the pressure gradients effectively choke nc v;'.
Q3. What is the limiting factor in the decay of a neutron star's magnetic field?
Should Hall drift be the limiting factor in the decay of a neutron star's magnetic field, the field strengths would decline approximately at t -1, as least while ~ B ~ 1.
Q4. What is the effect of the ohmic field on the crust?
Note that, if the magnetic field as well as the currents that support it is confined to the crust, the surface field strength would be about an order of magnitude smaller than the crustal field strength.
Q5. How does Pethick measure the residual strength of the surface field?
The residual strength of the surface field would be related to that in the inner core by (R;/ R)3 , where R; is the radius of the inner core.
Q6. What is the ratio of the number of charged particles to neutrons?
The stratification is associated with the chemical composition gradient; the equilibrium ratio of the number densities of charged particles to neutrons increases with depth.
Q7. Who were the first to properly calculate the ohmic decay time in the fluid core?
Pethick, & Pines (1969b) were the first to properly calculate the ohmic decay time in the fluid core under the assumption that the neutrons and protons were normal (not superfluid and superconducting).
Q8. Why do the authors neglect thermal contributions to the Brunt-ViiisiiHi frequency?
The authors neglect thermal contributions to the Brunt-ViiisiiHi frequency on the grounds that the thermal conductivity of neutron star interiors is so high that they are unimportant for the slow motions of interest here.
Q9. What is the buoyancy force density of a neutron star?
The buoyancy force density is to be compared to B2/(8nL), the characteristic magnitude of the force density associated with a magnetic field of scale L. Since L ;S H in the fluid core of a neutron star, the addition of buoyancy forces does not alter the time scales for ambipolar diffusion given by equations (34) and (35).
Q10. What is the reason for the decay of neutron stars?
Since the neutron stars found in recycled pulsars and low-mass X-ray binaries have accreted substantial amounts of matter, it is difficult to resolve whether the decay results from age or accretion (Bisnovatyi-Kogan & Kornberg 1975).
Q11. What is the only displacement of practical interest?
The authors show in§ 5 that the interactions which smooth perturbations of chemical equilibrium are so slow that these are the only displacements of practical interest.
Q12. What is the dispersion relation for linear waves in a uniform magnetic field?
To obtain the dispersion relation for linear waves in a uniform magnetic field B0 , the authors substitute the elementary disturbance B 1 = 1 1 exp i(k · x - wt) into equation (39).
Q13. Why is vir more complicated than f?
Because vir perturbs the chemical equilibrium between the neutrons and charged particles, its response to f~ is more complicated.
Q14. What is the effect of a composition gradient on the solenoidal component of the charged particle?
A composition gradient in the charged particle fraction of the core fluid would impede the solenoidal component of the charged particle flux.
Q15. What is the time scale for ohmic decay?
The time scale for ohmic decay, which follows immediately from equations (15) and (16), has the familiar form,...., 4nu0 13 tohmic 2 · c(33)Ohmic decay involves a diffusion of the magnetic field lines with respect to the charged particles.
Q16. What is the effect of exotic species on the stability of neutron stars?
The presence of exotic species of particles would affect the static stability of neutron star interiors as measured by the Brunt-ViiisiiHi frequency.