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We compare dynamics and waveforms from binary neutron star coalescence as computed by new long-term ($\sim 10 $ orbits) numerical relativity simulations and by the tidal effective-one-body (EOB) model including analytical tidal corrections up to second post-Newtonian order (2PN).
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1983
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2009
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2011
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2010
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T. Damour and A. Nagar, Phys.Rev. D81
2010
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J. E. Vines and E. E. Flanagan(2010), arXiv:1009.4919 [gr-qc]
2010
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L. Baiotti, T. Damour, B. Giacomazzo, A. Nagar, and L. Rezzolla, Phys.Rev.Lett. 105
2010
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J. Vines, E. E. Flanagan, and T. Hinderer, Phys.Rev. D83
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S. Bernuzzi, M. Thierfelder, and B. Brügmann(2011), arXiv:1109.3611 [gr-qc]
2011
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2012
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D. Bini, T. Damour, and G. Faye(2012), arXiv:1202.3565 [gr-qc]
2012
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T. Damour, A. Nagar, D. Pollney, and C. Reisswig, Phys.Rev.Lett. 108
2012
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J. A. Faber and F. A. Rasio(2012), arXiv:1204.3858 [gr-qc]
2012
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T. Damour, A. Nagar, D. Pollney, and C. Reisswig, in preparation(2012)
2012
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