Gravitational waves from hot young rapidly rotating neutron stars

Owen, B. J.; Lindblom, Lee; Cutler, Curt; Schutz, B. F.; Vecchio, A.; Andersson, Nils

doi:10.1103/physrevd.58.084020

Cited by 462 publications

(843 citation statements)

References 25 publications

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“…However, as was shown by Andersson (1998) and Friedman & Morsink (1998), rapidly rotating NSs are subject to gravitation-driven instability associated with enhancement of r-modes (toroidal oscillation mode of rotating star controlled by Coriolis force). It is a particular case of the ChandrasekharFriedman-Schutz (CFS) instability [Chandrasekhar 1970;Friedman & Schutz 1978a,b].…”

Section: Introductionmentioning

confidence: 99%

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Differential rotation and r-modes in magnetized neutron stars

Chugunov

2015

Monthly Notices of the Royal Astronomical Society

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] draw attention to the second order secular drift associated with r-modes and claimed that it should lead to magnetic field enhancement and suppression of r-mode instability in magnetized neutron stars. We critically revise these results. We present a particular second order r-mode solution with vanishing secular drift, thus refuting a widely believed statement that secular drift is an unavoidable feature of r-modes. This non-drifting solution is not affected by magnetic field B, if B ≪ B crit ≈ 10 17 (ν/600 Hz) G (ν is a spin frequency) and does not lead to secular evolution of magnetic field. For general second order r-mode solution the drift does not necessarily vanish, but the solution can be presented as a superposition of two solutions: one describes evolution of differential rotation in nonoscillating star (which describes secular drift; for nonmagnetized star it is arbitrary stationary rotation stratified on cylinders; for magnetized star differential rotation evolves on the Alfvén timescale and may lead to magnetic energy enhancement), and another one is non-drifting r-mode solution mentioned above. This representation allows us to conclude that enhancement of magnetic field energy is limited by initial energy of differential rotation, which is much less (for a factor ∝ α 2 , where α is mode amplitude) than the total energy of r-mode. Hence, magnetic field enhancement by drift cannot suppress r-mode instability. Results can be generalized for any oscillation mode in any medium, if this mode has non-drifting solution for B = 0.

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Section: Introductionmentioning

confidence: 99%

“…]. 5 We use normalization of the mode amplitude from Owen et al (1998), which is usually applied for r-mode instability analysis. Sá (2004); Sá & Tomé (2005) apply slightly different normalization, namely their amplitude…”

Section: R-modes In Nonmagnetized Nsmentioning

confidence: 99%

Differential rotation and r-modes in magnetized neutron stars

Chugunov

2015

Monthly Notices of the Royal Astronomical Society

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“…Haskell 2015 for a recent review). The standard model of r-mode instability (suggested by Lindblom, Owen & Morsink 1998;Owen et al 1998, see also Gusakov, Chugunov & Kantor 2014a for discussion of recent microphysical updates) assumes a hadronic composition of the NS core and dissipation by shear and bulk viscosity. It stabilizes the NS in the grey region in Fig.…”

Section: Upper Limit For Surface Temperature Of Msp 47 Tuc Aa and Conmentioning

confidence: 99%

Chandra studies of the globular cluster 47 Tucanae: a deeper X-ray source catalogue, five new X-ray counterparts to millisecond radio pulsars and new constraints to r-mode instability window

Bhattacharya

Heinke

Chugunov

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We combined Chandra ACIS observations of the globular cluster 47 Tucanae (hereafter, 47 Tuc) from 2000, 2002, and 2014-15 to create a deeper X-ray source list, and study some of the faint radio millisecond pulsars (MSPs) present in this cluster. We have detected 370 X-ray sources within the half-mass radius (2 .79) of the cluster, 81 of which are newly identified, by including new data and using improved source detection techniques. The majority of the newly identified sources are in the crowded core region, indicating cluster membership. We associate five of the new X-ray sources with chromospherically active BY Dra or W UMa variables identified by Albrow et al. (2001). We present alternative positions derived from two methods, centroiding and image reconstruction, for faint, crowded sources. We are able to extract X-ray spectra of the recently discovered MSPs 47 Tuc aa, 47 Tuc ab, the newly timed MSP 47 Tuc Z, and the newly resolved MSPs 47 Tuc S and 47 Tuc F. Generally, they are well fit by black body or neutron star atmosphere models, with temperatures, luminosities and emitting radii similar to those of other known MSPs in 47 Tuc, though 47 Tuc aa and 47 Tuc ab reach lower X-ray luminosities. We limit X-ray emission from the full surface of the rapidly spinning (542 Hz) MSP 47 Tuc aa, and use this limit to put an upper bound for amplitude of r-mode oscillations in this pulsar as α < 2.5 × 10 −9 and constrain the shape of the r-mode instability window.

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“…A stochastic background can be created in the early Universe following inflation [5][6][7][8], during a phase transition [4], or from cosmic strings [9][10][11][12][13][14] to name a few scenarios. Less speculative astrophysical stochastic backgrounds are expected to arise from more vanilla objects such as compact binaries [15][16][17][18][19], neutron stars [20][21][22][23][24][25][26][27][28], core collapse supernovae [29][30][31][32], white dwarf binaries [33] and supermassive black hole binaries [34][35][36].…”

Section: Introductionmentioning

confidence: 99%

Statistical properties of astrophysical gravitational-wave backgrounds

2014

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We investigate how a stochastic gravitational-wave background, produced from a discrete set of astrophysical sources, differs from an idealized model consisting of an isotropic, unpolarized, and Gaussian background. We focus, in particular, on the different signatures produced from these two cases, as observed in a cross-correlation search. We show that averaged over many realizations of an astrophysical background, the cross-correlation measurement of an astrophysical background is identical to that of an idealized background. However, any one realization of an astrophysical background can produce a different signature. Using a model consisting of an ensemble of binary neutron star coalescences, we quantify the typical difference between the signal from individual realizations of the astrophysical background and the idealized case. For advanced detectors, we find that, using a cross-correlation analysis, astrophysical backgrounds from many discrete sources are probably indistinguishable from an idealized background.

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Gravitational waves from hot young rapidly rotating neutron stars

Cited by 462 publications

References 25 publications

Differential rotation and r-modes in magnetized neutron stars

Differential rotation and r-modes in magnetized neutron stars

Chandra studies of the globular cluster 47 Tucanae: a deeper X-ray source catalogue, five new X-ray counterparts to millisecond radio pulsars and new constraints to r-mode instability window

Statistical properties of astrophysical gravitational-wave backgrounds

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