Details
| Original language | English |
|---|---|
| Article number | 061104 |
| Number of pages | 12 |
| Journal | Physical review letters |
| Volume | 122 |
| Issue number | 6 |
| Publication status | Published - 13 Feb 2019 |
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.
ASJC Scopus subject areas
- Physics and Astronomy(all)
- General Physics and Astronomy
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In: Physical review letters, Vol. 122, No. 6, 061104, 13.02.2019.
Research output: Contribution to journal › Article › Research
}
TY - JOUR
T1 - Constraining the p-Mode-g-Mode Tidal Instability with GW170817
AU - The LIGO Scientific Collaboration
AU - The Virgo Collaboration
AU - Abbott, Benjamin P.
AU - Abbott, Richard
AU - Abbott, T. D.
AU - Acernese, Fausto
AU - Ackley, K.
AU - Adams, C.
AU - Adams, T.
AU - Addesso, P.
AU - Adhikari, R. X.
AU - Adya, Vaishali
AU - Affeldt, Christoph
AU - Agarwal, Bhanu
AU - Agathos, Michalis
AU - Agatsuma, Kazuhiro
AU - Aggarwal, Nikhil
AU - Aguiar, Odylio Denys
AU - Aiello, Lorenzo
AU - Ain, A.
AU - Ajith, Parameswaran
AU - Allen, Bruce
AU - Allen, Gabrielle
AU - Bose, Susmita
AU - Brown, D. D.
AU - Chen, Y.
AU - Cheng, H. P.
AU - Danilishin, Shtefan
AU - Danzmann, Karsten
AU - Hanke, Marcus
AU - Hennig, J.
AU - Heurs, Michele
AU - Hreibi, A.
AU - Kumar, S.
AU - Lee, H. K.
AU - Li, X.
AU - Lück, Harald
AU - Nguyen, Truc T.
AU - Schmidt, P.
AU - Steinmeyer, Daniel
AU - Sun, L.
AU - Vahlbruch, Henning Fedor Cornelius
AU - Wang, Y. F.
AU - Wei, Li-Wei
AU - Wilken, Dennis Max
AU - Willke, Benno
AU - Wittel, Holger
AU - Zhang, L.
AU - Zhang, Yin
AU - Zhou, M.
AU - Aufmuth, Peter
AU - Bensch, Maximilian
AU - Bergmann, Gerald
AU - Bisht, Aparna
AU - Bode, Nina
AU - Booker, P.
AU - Brinkmann, Maximilian
AU - Denker, Timo
AU - de Varona, O.
AU - Doravari, S.
AU - Dreissigacker, C.
AU - Eggenstein, H.-B.
AU - Hochheim, S.
AU - Junker, J.
AU - Karvinen, Kai S.
AU - Kaufer, Stefan
AU - Kirchhoff, R.
AU - Koch, Patrick
AU - Köhlenbeck, S. M.
AU - Kringel, Volker
AU - Kuehn, G.
AU - Leavey, S.
AU - Lehmann, J.
AU - Leonardi, M.
AU - Mehmet, Moritz
AU - Mendoza-Gandara, D.
AU - Ming, J.
AU - Mukherjee, Arunava
AU - Nery, M.
AU - Ohme, F.
AU - Oppermann, P.
AU - Papa, M. A.
AU - Puncken, O.
AU - Schreiber, Emil
AU - Schütte, Dirk
AU - Schulte, B. W.
AU - Steinke, M.
AU - Steltner, B.
AU - Theeg, Thomas
AU - Thies, Fabian
AU - Weinert, Michael
AU - Wellmann, F.
AU - Weßels, Peter
AU - Wimmer, Maximilian H.
AU - Winkler, W.
AU - Woehler, J.
AU - Zhu, S. J.
AU - Lough, James
AU - Rüdiger, Albrecht
AU - Pal-Singh, A.
AU - Wu, D. S.
N1 - Funding information: 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.
PY - 2019/2/13
Y1 - 2019/2/13
N2 - 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.
AB - 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.
UR - http://www.scopus.com/inward/record.url?scp=85061565461&partnerID=8YFLogxK
U2 - 10.1103/PhysRevLett.122.061104
DO - 10.1103/PhysRevLett.122.061104
M3 - Article
C2 - 30822067
AN - SCOPUS:85061565461
VL - 122
JO - Physical review letters
JF - Physical review letters
SN - 0031-9007
IS - 6
M1 - 061104
ER -