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Dynamics Around Supermassive Black Holes: Extreme-mass-ratio Inspirals as Gravitational-wave Sources

  • Authors: Barak Rom, Itai Linial, Karamveer Kaur, Re'em Sari

Barak Rom et al 2024 The Astrophysical Journal 977 .

  • Provider: AAS Journals

Caption: Figure 4.

EMRI eccentricity probability density function at the mostly bound orbit. The blue line corresponds to the case where the sBH number fraction is larger than the critical value, ﹩{{\rm{f}}}_{\bullet }\geqslant {f}_{\bullet }^{c}﹩, where the distribution is independent of the specific value of f , and peaks at e ≃ 0.08. The red line exhibits an example of the complementary case, ﹩{{\rm{f}}}_{\bullet }={10}^{-5}\lt {f}_{\bullet }^{c}﹩, where the distribution peaks at e I ≃ 0.04 (as given by Equation (29)) and falls steeply, as ﹩p(e\gtrsim {e}_{I})\mathop{\propto }\limits_{\sim }{e}^{-49/19}﹩. In both cases, the distributions satisfy p(e ≪ 1) ∝ e 5/19.

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