David Radice, Sebastiano Bernuzzi, and Christian D. Ott,
Phys. Rev. D. 94, 064011 (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 ~10 ms and persists over secular timescales. Gravitational waves emitted by the m=1 instability have a peak frequency around 1−2 kHz 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. |
You can read more about this paper on David Radice's homepage at http://www.tapir.caltech.edu/~david_e/
The Gravitational Waveforms generated by our simulations are available (and citable!) on zenodo.org at http://dx.doi.org/10.5281/zenodo.46733.