Stochastic Gravitational Wave Background from Neutron Star r-mode Instability Revisited - INSPIRE

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Stochastic Gravitational Wave Background from Neutron Star r-mode Instability Revisited

Xing-Jiang Zhu
(
- Beijing Normal U.
)
,
Xi-Long Fan
(
- Trieste U. and
- Trieste Observ.
)
,
Zong-Hong Zhu
(
- Beijing Normal U.
)

Feb, 2011

28 pages

Published in:

Astrophys.J. 729 (2011) 59

e-Print:

1102.2786 [astro-ph.CO]

DOI:

10.1088/0004-637X/729/1/59

View in:

ADS Abstract Service

reference search41 citations

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Abstract: (arXiv)

We revisit the possibility and detectability of a stochastic gravitational wave background (SGWB) produced by a cosmological population of newborn neutron stars (NSs) with r-mode instabilities. We show that the resultant SGWB is insensitive to the choice of CSFR models, but depends strongly on the evolving behavior of CSFR at low redshifts. Our results show that the dimensionless energy density

\Omega_{\rm{GW}}

could have a peak amplitude of

\simeq (1-3.5) \times10^{-8}

in the frequency range

(200-1000)

~Hz. However, such a high mode amplitude is unrealistic as it is known that the maximum value is much smaller and at most

10^{-2}

. A realistic estimate of

\Omega_{\rm{GW}}

should be at least 4 orders of magnitude lower (

\sim 10^{-12}

), which leads to a pessimistic outlook for the detection of r-mode background. We consider different pairs of terrestrial interferometers (IFOs) and compare two approaches to combine multiple IFOs in order to evaluate the detectability of this GW background. Constraints on the total emitted GW energy associated with this mechanism to produce a detectable stochastic background are

\sim 10^{-3} M_{\odot} c^2

for two co-located advanced LIGO detectors, and

2 \times 10^{-5} M_{\odot} c^2

for two Einstein Telescopes. These constraints may also be applicable to alternative GW emission mechanisms related to oscillations or instabilities in NSs depending on the frequency band where most GWs are emitted.

gravitational waves
stars: neutron
stars: formation
supernovae: general
background: stochastic
gravitational radiation: stochastic
neutron star: formation
neutron star: stability
sensitivity
redshift

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