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https://hdl.handle.net/2440/118258
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Type: | Journal article |
Title: | Constraining the p-Mode-g-Mode Tidal Instability with GW170817 |
Author: | Abbott, B.P. Abbott, R. Abbott, T.D. Acernese, F. Ackley, K. Adams, C. Adams, T. Addesso, P. Adhikari, R.X. Adya, V.B. Affeldt, C. Agarwal, B. Agathos, M. Agatsuma, K. Aggarwal, N. Aguiar, O.D. Aiello, L. Ain, A. Ajith, P. Allen, B. et al. |
Citation: | Physical Review Letters, 2019; 122(6):061104-1-061104-12 |
Publisher: | American Physical Society |
Issue Date: | 2019 |
ISSN: | 0031-9007 1079-7114 |
Statement of Responsibility: | B. P. Abbot ... Miftar Ganija … Won Kim … Jesper, Munch … David J. Ottaway … Peter J. Veitch … et al. |
Abstract: | We analyze the impact of a proposed tidal instability coupling p modes and g modes within neutron stars on GW170817. This nonresonant instability transfers energy from the orbit of the binary to internal modes of the stars, accelerating the gravitational-wave driven inspiral. We model the impact of this instability on the phasing of the gravitational wave signal using three parameters per star: an overall amplitude, a saturation frequency, and a spectral index. Incorporating these additional parameters, we compute the Bayes factor (lnB_{!pg}^{pg}) comparing our p-g model to a standard one. We find that the observed signal is consistent with waveform models that neglect p-g effects, with lnB_{!pg}^{pg}=0.03_{-0.58}^{+0.70} (maximum a posteriori and 90% credible region). By injecting simulated signals that do not include p-g effects and recovering them with the p-g model, we show that there is a ≃50% probability of obtaining similar lnB_{!pg}^{pg} even when p-g effects are absent. We find that the p-g amplitude for 1.4 M_{⊙} neutron stars is constrained to less than a few tenths of the theoretical maximum, with maxima a posteriori near one-tenth this maximum and p-g saturation frequency ∼70 Hz. This suggests that there are less than a few hundred excited modes, assuming they all saturate by wave breaking. For comparison, theoretical upper bounds suggest ≲10^{3} modes saturate by wave breaking. Thus, the measured constraints only rule out extreme values of the p-g parameters. They also imply that the instability dissipates ≲10^{51} erg over the entire inspiral, i.e., less than a few percent of the energy radiated as gravitational waves. |
Keywords: | LIGO Scientific Collaboration and Virgo Collaboration |
Rights: | © 2019 American Physical Society |
DOI: | 10.1103/PhysRevLett.122.061104 |
Grant ID: | ARC |
Published version: | http://dx.doi.org/10.1103/physrevlett.122.061104 |
Appears in Collections: | Aurora harvest 8 Physics publications |
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