Gravitational wave constraints on the shape of neutron stars

Johnson-McDaniel, Nathan K.

doi:10.1103/physrevd.88.044016

Cited by 18 publications

(18 citation statements)

References 64 publications

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“…This is still the maximum observed spin-up for any globular cluster pulsar. 164 For this we have assumed a 1.4  M star and used approximate scalings calculated from Table 1 of Johnson-McDaniel (2013), taking into account that the rotational deformation scales with f rot 2 .…”

Section: Discussionmentioning

confidence: 99%

“…When the spin-down limit is not surpassed, no power ratio,˙Ė E gw , is given. a This is the equivalent upper limit on the = = l m 2 surface deformation maximized over the equation of state and stellar mass (Johnson-McDaniel 2013). Values below 10 are rounded to the nearest integer, values between 10 and 1000 are rounded to the nearest decade, and values above 1000 are rounded to the nearest hundred.…”

Section: Discussionmentioning

confidence: 99%

“…We also find that for five of these pulsars (PSRs J0534+2200, J1302−6350, J1813−1246, J1952+3252, and J2229+6114) the = = l m 2 surface deformations are smaller than the rotational (l = 2, m = 0) surface deformation for all equations of state. 164 For the Vela pulsar (PSR J0835−4510) and PSR J0205+6449, the = = l m 2 surface deformations are smaller than the rotational deformations for roughly half of the equations of state used in Johnson-McDaniel (2013). There is no expected relation between the scales of these two deformations, but it is intriguing to compare them nonetheless.…”

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confidence: 99%

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First Search for Gravitational Waves from Known Pulsars with Advanced LIGO

Abbott¹,

Abbott²,

Abbott³

et al. 2017

ApJ

156

186

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We present the result of searches for gravitational waves from 200 pulsars using data from the first observing run of the Advanced LIGO detectors. We find no significant evidence for a gravitational-wave signal from any of these pulsars, but we are able to set the most constraining upper limits yet on their gravitational-wave amplitudes and ellipticities. For eight of these pulsars, our upper limits give bounds that are improvements over the indirect spin-down limit values. For another 32, we are within a factor of 10 of the spin-down limit, and it is likely that some of these will be reachable in future runs of the advanced detector. Taken as a whole, these new results improve on previous limits by more than a factor of two.

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Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

mentioning

confidence: 99%

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First Search for Gravitational Waves from Known Pulsars with Advanced LIGO

Abbott¹,

Abbott²,

Abbott³

et al. 2017

ApJ

156

186

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“…maximum stress, which the elastically deformed crustal material can withstand). If the crust is indeed as strong as it is suggested by molecular dynamic (MD) sim-⋆ E-mail:baiko@astro.ioffe.ru † E-mail:andr@astro.ioffe.ru ulations (Horowitz & Kadau 2009;Chugunov & Horowitz 2010, the GW emission can be poweful enough to be detectable by existing GW observatories (Johnson-McDaniel 2013;Caplan & Horowitz 2017). Haskell & Patruno (2017) have recently suggested that this GW emission could be responsible for observed spin-down during the accreting phase of PSR J1023+0038.…”

Section: Introductionmentioning

confidence: 99%

Breaking properties of neutron star crust

Baiko

Chugunov

2018

Monthly Notices of the Royal Astronomical Society

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The strength of neutron star crust is crucial for modelling magnetar flares, pulsar glitches and gravitational wave emission. We aim to shed some light on this problem by analysing uniaxial stretch deformation (elongation and contraction) of perfect bodycentered cubic Coulomb crystals, paying special attention to the inherent anisotropy of this process. Our analysis is based on the semi-analytical approach of Baiko & Kozhberov (2017), which, for any uniform deformation, allows one to calculate, in fully non-linear regime, critical deformation parameters beyond which the lattice loses its dynamic stability. We determine critical strain, pressure anisotropy and deformation energy for any stretch direction with respect to the crystallographic axes. These quantities are shown to be strongly anisotropic: they vary by a factor of almost 10 depending on the orientation of the deformation axis. For polycrystalline crust, we argue that the maximum strain for the stretch deformation sustainable elastically is 0.04. It is lower than the breaking strain of 0.1 obtained in molecular dynamic simulations of a shear deformation by Horowitz & Kadau (2009). The maximum pressure anisotropy of polycrystalline matter is estimated to be in the range from 0.005 to 0.014 nZ 2 e 2 /a, where n is the ion number density, Ze is the ion charge, and a is the ion-sphere radius. We discuss possible mechanisms of plastic motion and formation of large crystallites in neutron star crust as well as analyse energy release associated with breaking of such crystallites in the context of magnetic field evolution and magnetar flaring activity.

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“…Second and third columns: Median of the 95% confidence level UL on the GW amplitude h 0 and corresponding ellipticity ϵ. Fourth column: Surface deformation corresponding to the median ellipticity for a NS with radius of 10 km[53]. Fifth column: Ratio between the median UL and the spin-down limit.…”

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confidence: 99%

Narrow-band search for gravitational waves from known pulsars using the second LIGO observing run

Abbott¹,

Abbott²,

Abbott³

et al. 2019

Phys. Rev. D

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Isolated spinning neutron stars, asymmetric with respect to their rotation axis, are expected to be sources of continuous gravitational waves. The most sensitive searches for these sources are based on accurate matched filtering techniques that assume the continuous wave to be phase locked with the pulsar beamed emission. While matched filtering maximizes the search sensitivity, a significant signal-to-noise ratio loss will happen in the case of a mismatch between the assumed and the true signal phase evolution. Narrowband algorithms allow for a small mismatch in the frequency and spin-down values of the pulsar while coherently integrating the entire dataset. In this paper, we describe a narrow-band search using LIGO O2 data for the continuous wave emission of 33 pulsars. No evidence of a continuous wave signal is found, and upper limits on the gravitational wave amplitude over the analyzed frequency and spin-down ranges are computed for each of the targets. In this search, we surpass the spin-down limit, namely, the maximum rotational energy loss due to gravitational waves emission for some of the pulsars already present in the

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Gravitational wave constraints on the shape of neutron stars

Cited by 18 publications

References 64 publications

First Search for Gravitational Waves from Known Pulsars with Advanced LIGO

First Search for Gravitational Waves from Known Pulsars with Advanced LIGO

Breaking properties of neutron star crust

Narrow-band search for gravitational waves from known pulsars using the second LIGO observing run

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