Amplitude modulation in binary gravitational lensing of gravitational waves

Qiu, Yi; Wang, Ke; He, Jifeng

doi:10.48550/arxiv.2205.01682

Cited by 1 publication

(1 citation statement)

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“…Future work should consider the tensor diffraction formula [44] and its polarizations [45]. He et al [46][47][48][49] have simulated GW lensing systems in their studies. To obtain more accurate lensed GW waveforms in such scenarios and to assess the accuracy of our diffraction formula, further simulations and research are warranted.…”

Section: Discussionmentioning

confidence: 99%

Testing an exact diffraction formula with gravitational wave source lensed by a supermassive black hole in binary systems

Guo,

Cao

2024

J. Cosmol. Astropart. Phys.

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When it comes to long-wavelength gravitational waves (GWs), diffraction effect becomes significant when these waves are lensed by celestial bodies. Typically, the traditional diffraction integral formula neglects large-angle diffraction, which is often adequate for most of cases. Nonetheless, there are specific scenarios, such as when a GW source is lensed by a supermassive black hole in a binary system, where the lens and source are in close proximity, where large-angle diffraction can play a crucial role. In our prior research, we have introduced an exact, general diffraction integral formula that accounts for large-angle diffraction as well. This paper explores the disparities between this exact diffraction formula and the traditional, approximate one under various special conditions. Our findings indicate that, under specific parameters — such as a lens-source distance of D LS = 0.1 AU and a lens mass of M L = 4 × 106 M ⊙ — the amplification factor for the exact diffraction formula is notably smaller than that of the approximate formula, differing by a factor of approximately rF ≃ 0.806. This difference is substantial enough to be detectable. Furthermore, our study reveals that the proportionality factor rF gradually increases from 0.5 to 1 as D LS increases, and decreases as M L increases. Significant differences between the exact and approximate formulas are observable when D LS ≲ 0.2 AU (assuming M L = 4 × 106 M ⊙) or when M L ≳ 2 × 106 M ⊙ (assuming D LS = 0.1 AU). These findings suggest that there is potential to validate our general diffraction formula through future GW detections.

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