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https://hdl.handle.net/2440/118258
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dc.contributor.author | Abbott, B.P. | - |
dc.contributor.author | Abbott, R. | - |
dc.contributor.author | Abbott, T.D. | - |
dc.contributor.author | Acernese, F. | - |
dc.contributor.author | Ackley, K. | - |
dc.contributor.author | Adams, C. | - |
dc.contributor.author | Adams, T. | - |
dc.contributor.author | Addesso, P. | - |
dc.contributor.author | Adhikari, R.X. | - |
dc.contributor.author | Adya, V.B. | - |
dc.contributor.author | Affeldt, C. | - |
dc.contributor.author | Agarwal, B. | - |
dc.contributor.author | Agathos, M. | - |
dc.contributor.author | Agatsuma, K. | - |
dc.contributor.author | Aggarwal, N. | - |
dc.contributor.author | Aguiar, O.D. | - |
dc.contributor.author | Aiello, L. | - |
dc.contributor.author | Ain, A. | - |
dc.contributor.author | Ajith, P. | - |
dc.contributor.author | Allen, B. | - |
dc.contributor.author | et al. | - |
dc.date.issued | 2019 | - |
dc.identifier.citation | Physical Review Letters, 2019; 122(6):061104-1-061104-12 | - |
dc.identifier.issn | 0031-9007 | - |
dc.identifier.issn | 1079-7114 | - |
dc.identifier.uri | http://hdl.handle.net/2440/118258 | - |
dc.description.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. | - |
dc.description.statementofresponsibility | B. P. Abbot ... Miftar Ganija … Won Kim … Jesper, Munch … David J. Ottaway … Peter J. Veitch … et al. | - |
dc.language.iso | en | - |
dc.publisher | American Physical Society | - |
dc.rights | © 2019 American Physical Society | - |
dc.source.uri | http://dx.doi.org/10.1103/physrevlett.122.061104 | - |
dc.subject | LIGO Scientific Collaboration and Virgo Collaboration | - |
dc.title | Constraining the p-Mode-g-Mode Tidal Instability with GW170817 | - |
dc.type | Journal article | - |
dc.identifier.doi | 10.1103/PhysRevLett.122.061104 | - |
dc.relation.grant | ARC | - |
pubs.publication-status | Published | - |
dc.identifier.orcid | Cao, H. [0000-0001-6583-6907] | - |
dc.identifier.orcid | Ganija, M. [0000-0002-6882-3930] | - |
dc.identifier.orcid | Ingram, C. [0000-0003-0152-3279] | - |
dc.identifier.orcid | Ng, S. [0000-0001-5843-1434] | - |
dc.identifier.orcid | Ottaway, D. [0000-0001-6794-1591] | - |
dc.identifier.orcid | Veitch, P. [0000-0002-2597-435X] | - |
Appears in Collections: | Aurora harvest 8 Physics publications |
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