Abbott, B. P. and Abbott, R. and Adhikari, R. X. and Ananyeva, A. and Anderson, S. B. and Appert, S. and Arai, K. and Araya, M. C. and Barayoga, J. C. and Barish, B. C. and Berger, B.K. and Billingsley, G. and Biscans, S. and Blackburn, J. K. and Bork, R. and Brooks, A. F. and Brunett, S. and Cahillane, C. and Callister, T. A. and Cepeda, C. B. and Coughlin, M. W. and Couvares, P. and Coyne, D. C. and Ehrens, P. and Eichholz, J. and Etzel, T. and Feicht, J. and Gossan, S. E. and Gushwa, K.E. and Gustafson, E. K. and Heptonstall, A. W. and Hulko, M. and Isi, M. and Kamai, B. and Kanner, J. B. and Kondrashov, V. and Korth, W. Z. and Kozak, D. B. and Lazzarini, A. and Markowitz, A. and Maros, E. and Massinger, T. J. and Matichard, F. and McIver, J. and Meshkov, S. and Nevin, L. and Pedraza, M. and Quintero, E. A. and Reitze, D. H. and Robertson, N. A. and Rollins, J. G. and Sachdev, S. and Sanchez, E. J. and Sanchez, L. E. and Taylor, R. and Torrie, C. I. and Urban, A. L. and Vajente, G. and Vass, S. and Venugopalan, G. and Wade, A. R. and Wallace, L. and Weinstein, A. J. and Williams, R. D. and Willis, J. L. and Wipf, C. C. and Xiao, S. and Yamamoto, H. and Zhang, L. and Zucker, M. E. and Zweizig, J. and Barkett, K. and Blackman, J. and Chen, Y. and Chua, A. J. K. and Li, X. and Ma, Y. and Pang, B. and Scheel, M. and Tso, R. and Varma, V. and Chatziioannou, K. (2019) Constraining the p-Mode–g-Mode Tidal Instability with GW170817. Physical Review Letters, 122 (6). Art. No. 061104. ISSN 0031-9007. doi:10.1103/PhysRevLett.122.061104. https://resolver.caltech.edu/CaltechAUTHORS:20190219-140840506
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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 (ln B^(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^(+0.70)_(−0.58) (maximum a posteriori and 90% credible region). By injecting simulated signals that do not include p−geffects 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.
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| Additional Information: | © 2019 American Physical Society. Received 13 September 2018; revised manuscript received 30 October 2018; published 13 February 2019. The authors gratefully acknowledge the support of the United States National Science Foundation (NSF) for the construction and operation of the LIGO Laboratory and Advanced LIGO as well as the Science and Technology Facilities Council (STFC) of the United Kingdom, the Max-Planck-Society (MPS), and the State of Niedersachsen, Germany for support of the construction of Advanced LIGO and construction and operation of the GEO600 detector. Additional support for Advanced LIGO was provided by the Australian Research Council. The authors gratefully acknowledge the Italian Istituto Nazionale di Fisica Nucleare (INFN), the French Centre National de la Recherche Scientifique (CNRS) and the Foundation for Fundamental Research on Matter supported by the Netherlands Organisation for Scientific Research, for the construction and operation of the Virgo detector and the creation and support of the EGO consortium. The authors also gratefully acknowledge research support from these agencies as well as by the Council of Scientific and Industrial Research of India, the Department of Science and Technology, India, the Science & Engineering Research Board (SERB), India, the Ministry of Human Resource Development, India, the Spanish Agencia Estatal de Investigación, the Vicepresidència i Conselleria d’Innovació, Recerca i Turisme and the Conselleria d’Educació i Universitat del Govern de les Illes Balears, the Conselleria d’Educació, Investigació, Cultura i Esport de la Generalitat Valenciana, the National Science Centre of Poland, the Swiss National Science Foundation (SNSF), the Russian Foundation for Basic Research, the Russian Science Foundation, the European Commission, the European Regional Development Funds (ERDF), the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, the Hungarian Scientific Research Fund (OTKA), the Lyon Institute of Origins (LIO), the Paris Île-de-France Region, the National Research, Development and Innovation Office Hungary (NKFI), the National Research Foundation of Korea, Industry Canada and the Province of Ontario through the Ministry of Economic Development and Innovation, the Natural Science and Engineering Research Council Canada, the Canadian Institute for Advanced Research, the Brazilian Ministry of Science, Technology, Innovations, and Communications, the International Center for Theoretical Physics South American Institute for Fundamental Research (ICTP-SAIFR), the Research Grants Council of Hong Kong, the National Natural Science Foundation of China (NSFC), the Leverhulme Trust, the Research Corporation, the Ministry of Science and Technology (MOST), Taiwan and the Kavli Foundation. The authors gratefully acknowledge the support of the NSF, STFC, MPS, INFN, CNRS and the State of Niedersachsen, Germany for provision of computational resources. N. Weinberg was supported in part by NASA Grant No. NNX14AB40G. | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Group: | LIGO, Astronomy Department | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
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| Issue or Number: | 6 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| DOI: | 10.1103/PhysRevLett.122.061104 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Record Number: | CaltechAUTHORS:20190219-140840506 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Persistent URL: | https://resolver.caltech.edu/CaltechAUTHORS:20190219-140840506 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
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| ID Code: | 92988 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Collection: | CaltechAUTHORS | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Deposited By: | Tony Diaz | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Deposited On: | 19 Feb 2019 22:52 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Last Modified: | 28 Apr 2023 20:26 |
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