Ultraviolet Emission from the Millisecond Pulsar J0437−4715

Kargaltsev, Oleg; Pavlov, G. G.; Romani, Roger W.

doi:10.1086/380993

Cited by 112 publications

(180 citation statements)

References 43 publications

(64 reference statements)

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“…Observations of a delayed response in the recovery after a glitch, over a timescale proportional to the glitch size as in (83) would, on the other hand, would provide a hint that vortex slippage is occurring in neutron stars. Finally let us note that vortex creep is a dissipative process and creep heating [21,[191][192][193] might explain the unusually high (for their age) temperatures that have been measured for some old, recycled millisecond pulsars, such as J0437-4715 [194] .…”

Section: A Vortex Slippagementioning

confidence: 99%

Models of pulsar glitches

Haskell

Melatos

2015

Int. J. Mod. Phys. D

317

304

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Radio pulsars provide us with some of the most stable clocks in the universe. Nevertheless several pulsars exhibit sudden spin-up events, known as glitches. More than forty years after their first discovery, the exact origin of these phenomena is still open to debate. It is generally thought that they an observational manifestation of a superfluid component in the stellar interior and provide an insight into the dynamics of matter at extreme densities. In recent years there have been several advances on both the theoretical and observational side, that have provided significant steps forward in our understanding of neutron star interior dynamics and possible glitch mechanisms. In this article we review the main glitch models that have been proposed and discuss our understanding, in the light of current observations.Radio pulsars are thought to be rotating magnetised neutron stars (NS). The huge moment of inertia (of the order of 10 45 g cm 2 ) leads to exceptionally stable rotation rates and provides us with some of the most precise clocks in the universe. The best timed millisecond pulsars are stable to a precision which rivals that of atomic clocks [1]. Nevertheless radio pulsars exhibit several timing irregularities, the most striking of which are the so-called glitches. While most objects are observed to steadily spin-down due to the emission of electromagnetic and, possibly, gravitational waves, many pulsars show sudden increases in their spin, in some cases followed by an increase in their spin-down rate, i.e. glitches. Most pulsars also show slower, long-term, stochastic deviations from a regular spin-down law, that are generally classed as 'timing noise' and are not the main focus of this review article.Soon after the discovery of the first glitches in the Vela [2,3] and Crab [4,5] pulsars in 1969, several mechanisms were suggested to explain these phenomena. Although some initial suggestions featured external mechanisms, such as plasma explosions in the magnetosphere [6] or planets around the pulsar [7], the lack of radiative and pulse profile changes associated with these events was taken as evidence for an internal origin. The situation is different for rotating radio transients (RRATs) and magnetars, which are now known to glitch and do exhibit, amongst other peculiar traits, radiative changes associated with these events [8][9][10][11]. Magnetospheric activity is likely to play a role in these objects, as we discuss below.There are two main internal glitch mechanisms that have been examined in the literature. The first set of models relies on the fact that the outer layers of a neutron star form a crystalline crust that can support stress. As the NS spins down, the liquid core adjusts its shape to the rotation rate, while the solid crust maintains the shape appropriate for the previous, higher, spin rate. This leads to an increasing amount of strain building up in the crust, which is eventually released in the form of a star quake. The quake causes a sudden rearrangement of the moment of inertia and...

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Section: A Vortex Slippagementioning

confidence: 99%

Models of pulsar glitches

Haskell

Melatos

2015

Int. J. Mod. Phys. D

317

304

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“…Examples of nearby neutron stars are J0437-4715 [24] and J0108-1431 [25] (140 pc and 130 pc from the Earth, respectively). The examples of neutron stars in globular clusters are e.g.…”

mentioning

confidence: 99%

Excluding Light Asymmetric Bosonic Dark Matter

Kouvaris¹,

Tinyakov²

2011

Phys. Rev. Lett.

172

236

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We argue that current neutron star observations exclude asymmetric bosonic non-interacting dark matter in the range from 2 keV to 16 GeV, including the 5-15 GeV range favored by DAMA and CoGeNT. If bosonic WIMPs are composite of fermions, the same limits apply provided the compositeness scale is higher than ∼ 10 12 GeV (for WIMP mass ∼ 1 GeV). In case of repulsive self-interactions, we exclude large range of WIMP masses and interaction cross sections which complements the constraints imposed by observations of the Bullet Cluster. Apart from direct searches, constraints on WIMPs can be set by observations of compact objects such as white dwarfs and neutron stars [4][5][6][7][8][9][10][11][12]. These constraints can be grouped in two types. The first type targets WIMPs that can annihilate inside the star producing heat that can change the thermal evolution of the star [5]. WIMPs of this type can arise in supersymmetric extensions of the SM (see [13] and references therein), or in Technicolor models [14]. Constraints of the second type target asymmetric DM models. In these models the annihilation of DM in the present-day Universe is impossible because only particles, and no anti-particles (hence the term "asymmetric") remain [15][16][17][18][19]. An additional bonus in these models is that the asymmetry of WIMPs might be linked through sphalerons with the baryon asymmetry [16,18], which can explain the today's ratio Ω DM /Ω B ∼ 5 provided the WIMP has a mass around 5 GeV. Note that this value is not far from the one suggested by DAMA and CoGeNT. In view of this coincidence, the models with WIMP masses in the GeV range have become quite popular.Since in the asymmetric DM models WIMPs cannot annihilate, if a large number of them is accreted during the lifetime of a neutron star, they may collapse forming a small black hole inside the star that eventually destroy the latter. Therefore the existence of old neutron stars can impose constraints on the properties of asymmetric WIMPs. In fact, in the case of fermionic asymmet-

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“…The value ofĠ is chosen so that predictions from the x = 0 EOS are just above the 90% confidence contour of Kargaltsev et al [22], see This observation has been already made in a previous work [52] in conjunction with a study of the neutron star radius and was interpreted in terms of the good agreement between the corresponding symmetry energies up to about 5ρ 0 (see also Fig. 2, lower frame).…”

Section: Constraining the Changing Rate Of The Gravitational Consmentioning

confidence: 56%

“…The stationary surface temperature in et al [22]. There are several possible reasons which could account for this discrepancy: (i)…”

Section: Constraining the Changing Rate Of The Gravitational Consmentioning

confidence: 89%

“…While the approach applied by Copi et al [70] probes the constancy of G over the age of Universe (see Table 1), the gravitochemical heating method is sensitive to variations in G over shorter periods [1,69], and falls closest to the second group of methods listed in Table 1. (ii) We do not consider the rotochemical heating [24] in this paper. On the other hand, the rotochemical heating, which is believed to play an important role in the thermal evolution of millisecond pulsars, cannot explain alone the observations of Kargaltsev et al [22]. Therefore, additional heating mechanisms need to be considered [24].…”

Section: Constraining the Changing Rate Of The Gravitational Consmentioning

confidence: 96%

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