Vortex creep and the internal temperature of neutron stars The Crab pulsar and PSR 0525 + 21

Alpar, M. A.; Nandkumar, Radha; Pines, David

doi:10.1086/162780

Cited by 47 publications

(28 citation statements)

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“…A star with viscous coupling between different internal components has to dissipate energy when it is spun up or down by an external torque. Reheating of neutron stars by energy dissipation was first considered by Alpar et al (1984Alpar et al ( , 1986 in connection with the dynamical coupling between the pinned inner crust superfluid and the crust of the neutron star. The steady state thermal luminosity supplied by energy dissipation is of the form:…”

Section: Energy Dissipationmentioning

confidence: 99%

Dim isolated neutron stars, cooling and energy dissipation

Alpar

2007

Astrophys Space Sci

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The cooling and reheating histories of dim isolated neutron stars (DINs) are discussed. Energy dissipation due to dipole spindown with ordinary and magnetar fields, and due to torques from a fallback disk are considered as alternative sources of reheating which would set the temperature of the neutron star after the initial cooling era. Cooling or thermal ages are related to the numbers and formation rates of the DINs and therefore to their relations with other isolated neutron star populations. The possibility of energy dissipation at ages greater than about 10 6 yrs is a potentially important factor in determining the properties of the DIN population. Interaction with a fallback disk, higher multipole fields and activity of the neutron star are briefly discussed.

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Section: Energy Dissipationmentioning

confidence: 99%

Dim isolated neutron stars, cooling and energy dissipation

Alpar

2007

Astrophys Space Sci

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“…The recovery is characterised by time-scales between 1 and 200 days, but it is incomplete in the sense that there is a persistent and cumulative increase in the spin-down rate (Lyne et al 1993). Alpar et al (1985) successfully applied the vortex creep model to the earlier Crab glitches and PSR B0525+21. They explained the persistent shift in (2.19) 5.…”

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confidence: 99%

Timing observations of southern pulsars - 1987 to 1991

D’Alessandro

McCulloch

King

et al. 1993

Monthly Notices of the Royal Astronomical Society

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Pulse arrival-time measurements made at frequencies near 670 and 800 MHz over a 7-year period have been used to study the timing behaviour of 45 southern pulsars. These measurements have resulted in more accurate estimates of the period, period derivative, position and dispersion measure of most of these pulsars. Changes in some of the dispersion measures have been detected and used to estimate the scale-sizes and electron densities of irregularities in the interstellar medium. The timing measurements also revealed distinct jumps in the rotation rate of five pulsars, most of which have not been reported elsewhere.Polarimetric data at 670 and 800 MHz are presented for eighteen of the more luminous pulsars. The integrated profiles display properties in general agreement with trends extrapolated from other frequencies. Rotation measures have been derived for these pulsars. Nine are more accurate than previous determinations, and two have changed since they were last measured. These changes suggest a dense, magnetised electron cloud has moved into or out of the line of sight.It has been confirmed that the level of pulsar timing noise is correlated with spin-down rates. Further analyses have revealed that, in most pulsars, the observed timing noise is due to a mixture of different kinds of activity, such as random walk processes, microjumps, and for one pulsar, free precession of the spin axis. The microjumps are characterised by a variety of signatures, involving both positive and negative changes in the rotation frequency and frequency derivative. The amplitudes of these microjumps form the tail-end of a continuous distribution of amplitudes extending down to microglitch level. An investigation of timing noise in the Vela pulsar has shown that the microactivity during the postglitch recovery period is dominated by microjumps in the rotation frequency and frequency derivative which occur every 30-40 days. This microactivity is also punctuated by less frequent events, such as large steps in the frequency derivative, discrete changes in the frequency second derivative, and in one isolated case, a small glitch. The above results have been discussed in terms of current theories of pulsar timing noise and it was found that no theoretical model, in isolation, is able to explain the range of observed timing activity in the pulsars studied.Power spectra of the pulsar timing residuals have been derived using a novel technique based on the CLEAN algorithm. Most of the spectra are well described by a single-or double-component power-law model. Some of these spectra can be interpreted in the context of one or more of the current timing noise models.

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“…Let us start by examining the salient features of a 1.4 solar mass (MO = 2 x 1033 g) "cold" neutron star with "stiff" equation of state, shown in Fig. 1 (from Pines and Alpar 1985). Going from outside to the centre, one encounters first an atmosphere a few meters thick, followed by an outer crust, a few hun dred meters in depth and of density increasing from 7 x 106 to 4 x 101 1 g/cm3.…”

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confidence: 99%

“…For the pur poses of a first order calculation, let us assume a two component thermodyna- Pines and Alpar (1985). mic model of a one solar mass neutron star: 1) an isothermal interior starting around the density   1010 g/cm3, within which almost all of the thermal energy resides; 2) an outer envelope starting with the surface and extending to the isothermal interior along which the temperature in creases from Ts of the surface to Tc of S C the interior (see Shapiro and Teukolsky 1983, Chapter 11 for a review of neutron star cooling).…”

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confidence: 99%

“…Alpar et al (1985) have develo ped a theory of vortex creep (movement of the quantized rotation of superfluid neutrons through the inner crust lattice) and interpreted the glitches in the rota tion rates of Crab and Vela pulsars. The internal temperature of the neutron star is one parameter in this model which, after theoretical estimates of the other parameters, can be fitted to the data.…”

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confidence: 99%

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