Gravitational Waves from Coalescing Binaries

Babak, S.

doi:10.1007/978-3-031-02612-6_2

Cited by 1 publication

(3 citation statements)

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“…The masses are given for the detector reference frame and are expressed in M e . Column 7 gives the post-Newtonian chirp masses corrected by using of the time lapse function α Kerr (23). Columns 4 and 8 give, respectively, the published source luminosity distances, D L GWTC and the corrected ones, D L c (both are in Gpc).…”

Section: Discussionmentioning

confidence: 99%

“…For our simplified calculations with the tidally locked blackholes, we compute the values α Kerr via formula (23) with the use of the metric components (25) g tt = 1 − r g /r, g jj = − (r 2 + a 2 + a 2 r g /r) and g tj = 2ar g /(rc 2 ) which are given in the 10th column of table 1. As one would expect, these values are smaller than the values α Sch for the static Schwarzschild metric (9th column of the same table).…”

Section: Angular Momentummentioning

confidence: 99%

“…Besides the analysis of the gravitational wave signal GW150914 by LVC [2], there are other works discussing properties of this signal from different points of view and with different purposes: see [19][20][21][22][23][24][25]. Here we shall return to the analysis of the same signal, with the purpose of clarifying the question posed by C M Will about how the linearised PN approximation of General Relativity (i.e.…”

Section: Introductionmentioning

confidence: 99%

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Two-body problem in curved spacetime: exploring gravitational wave transient cases

Yershov¹,

Raikov

Popova

2023

Phys. Scr.

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We explore gravitational-wave transient cases from the perspective of the two-body problem in curved spacetime, starting with the first case, GW150914, which marks the GW discovery [1]. In this paper, the LVC authors estimated the characteristic (chirp) mass of the binary blackhole system emitted this signal. Their calculation was based on Numerical-Relativity (NR) templates and presumably accounted fully for the non-linearity of GR. The same team later presented an alternative analysis of GW150914 [2], using the quadrupole post-Newtonian (PN) approximation of GR. Both analyses gave similar results, despite being based on quite different assumptions about the linearity or non-linearity of the coordinate reference frame near the GW source. Here we revisit the PN-analysis of GW150914. As in paper [2], our result also agrees with the NR-based chirp mass value published in [1]. Additionally, we apply the PN-approximation formalism to the rest of the GWTC cases, finding that practically all of their PN-approximated chirp masses coincide with the published NR-based values from GWTC. In our view, this implies that the NR-based theory, which is currently in use for processing GW signals, does not fully account for the difference between the source and detector reference frames because the PN-approximation, which is used for the comparison, does not account for this difference by design, given the flat-spacetime initial assumptions of this approximation. We find that the basis of this issue lies in the missing information about the derivatives of GW frequencies in the source reference frame. This leads to a systematic error in the estimated chirp masses of GW sources. The corresponding luminosity distances of these sources also turn out to be overestimated.

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Section: Discussionmentioning

confidence: 99%

Section: Angular Momentummentioning

confidence: 99%