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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 1.

Orbital dynamics in the (r, r p ) phase space, where r is the semimajor axis and r p is the periapsis. The dashed black line distinguishes between the two-body-scattering-dominated region and the GW-dominated one (Equation (7)); above it, the scattering leads to a diffusion dominantly in the r p -direction (as encapsulated by the shaded vertical blue funnel), while below it, GW emission efficiently shrinks and circularizes the orbit (along the horizontal shaded funnel). The red dashed–dotted line marks the mostly bound orbit, with r p = 4R s , and the yellow dashed–dotted line represents the critical semimajor axis R c , (Equation (8)), separating EMRI progenitors (with rR c ) and plunge progenitors (with rR c ). The gray lines demonstrate examples of trajectories leading to an EMRI or a plunge, according to their initial semimajor axis.

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