We study the development and saturation of the $m=1$ one-armed spiral instability in remnants of binary neutron star mergers by means of high-resolution long-term numerical relativity simulations. Our results suggest that this instability is a generic outcome of neutron stars mergers in astrophysically relevant configurations; including both "stiff" and "soft" nuclear equations of state. We find that, once seeded at merger, the $m=1$ mode saturates within $\sim 10\ \mathrmms$ and persists over secular timescales. Gravitational waves emitted by the $m=1$ instability have a peak frequency around $1-2\ \mathrmkHz$ and, if detected, could be used to constrain the equation of state of neutron stars. We construct hybrid waveforms spanning the entire Advanced LIGO band by combining our high-resolution numerical data with state-of-the-art effective-one-body waveforms including tidal effects. We use the complete hybrid waveforms to study the detectability of the one-armed spiral instability for both Advanced LIGO and the Einstein Telescope. We conclude that the one-armed spiral instability is not an efficient gravitational wave emitter. Its observation by current generation detectors is unlikely and will require third-generation interferometers.

One-armed spiral instability in neutron star mergers and its detectability in gravitational waves / Radice, David; Bernuzzi, Sebastiano; Ott, Christian D.. - In: PHYSICAL REVIEW D. - ISSN 2470-0010. - 94:6(2016). [10.1103/PhysRevD.94.064011]

One-armed spiral instability in neutron star mergers and its detectability in gravitational waves

BERNUZZI, Sebastiano;
2016

Abstract

We study the development and saturation of the $m=1$ one-armed spiral instability in remnants of binary neutron star mergers by means of high-resolution long-term numerical relativity simulations. Our results suggest that this instability is a generic outcome of neutron stars mergers in astrophysically relevant configurations; including both "stiff" and "soft" nuclear equations of state. We find that, once seeded at merger, the $m=1$ mode saturates within $\sim 10\ \mathrmms$ and persists over secular timescales. Gravitational waves emitted by the $m=1$ instability have a peak frequency around $1-2\ \mathrmkHz$ and, if detected, could be used to constrain the equation of state of neutron stars. We construct hybrid waveforms spanning the entire Advanced LIGO band by combining our high-resolution numerical data with state-of-the-art effective-one-body waveforms including tidal effects. We use the complete hybrid waveforms to study the detectability of the one-armed spiral instability for both Advanced LIGO and the Einstein Telescope. We conclude that the one-armed spiral instability is not an efficient gravitational wave emitter. Its observation by current generation detectors is unlikely and will require third-generation interferometers.
One-armed spiral instability in neutron star mergers and its detectability in gravitational waves / Radice, David; Bernuzzi, Sebastiano; Ott, Christian D.. - In: PHYSICAL REVIEW D. - ISSN 2470-0010. - 94:6(2016). [10.1103/PhysRevD.94.064011]
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Utilizza questo identificativo per citare o creare un link a questo documento: http://hdl.handle.net/11381/2814286
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