TY - JOUR
T1 - Dynamics Around Supermassive Black Holes
T2 - Extreme-mass-ratio Inspirals as Gravitational-wave Sources
AU - Rom, Barak
AU - Linial, Itai
AU - Kaur, Karamveer
AU - Sari, Re’em
N1 - Publisher Copyright:
© 2024. The Author(s). Published by the American Astronomical Society.
PY - 2024/12/1
Y1 - 2024/12/1
N2 - Supermassive black holes and their surrounding dense stellar environments nourish a variety of astrophysical phenomena. We focus on the distribution of stellar-mass black holes around the supermassive black hole and the consequent formation of extreme-mass-ratio inspirals (EMRIs). We derive a steady-state distribution, considering the effects of two-body scattering and gravitational-wave emission, and calculate the EMRI formation rate, eccentricity distribution, and EMRI-to-plunge ratio. Our model predicts: (a) a stronger segregation than previously estimated at the outskirts of the sphere of influence (at ∼0.01-2 pc for a Milky Way-like galaxy); (b) an increased EMRI-to-plunge ratio, favoring EMRIs at galaxies where stellar-mass black holes are scarce; (c) a detection of about 2 × 103 resolvable EMRIs, with a signal-to-noise ratio above 20, along a 4 yr LISA mission time; and (d) a confusion noise, induced by a cosmological population of unresolved EMRIs, reducing the LISA sensitivity in the 1-5 mHz frequency range by up to a factor of ≈2, relative to the instrumental noise.
AB - Supermassive black holes and their surrounding dense stellar environments nourish a variety of astrophysical phenomena. We focus on the distribution of stellar-mass black holes around the supermassive black hole and the consequent formation of extreme-mass-ratio inspirals (EMRIs). We derive a steady-state distribution, considering the effects of two-body scattering and gravitational-wave emission, and calculate the EMRI formation rate, eccentricity distribution, and EMRI-to-plunge ratio. Our model predicts: (a) a stronger segregation than previously estimated at the outskirts of the sphere of influence (at ∼0.01-2 pc for a Milky Way-like galaxy); (b) an increased EMRI-to-plunge ratio, favoring EMRIs at galaxies where stellar-mass black holes are scarce; (c) a detection of about 2 × 103 resolvable EMRIs, with a signal-to-noise ratio above 20, along a 4 yr LISA mission time; and (d) a confusion noise, induced by a cosmological population of unresolved EMRIs, reducing the LISA sensitivity in the 1-5 mHz frequency range by up to a factor of ≈2, relative to the instrumental noise.
UR - http://www.scopus.com/inward/record.url?scp=85210952025&partnerID=8YFLogxK
U2 - 10.3847/1538-4357/ad8b1d
DO - 10.3847/1538-4357/ad8b1d
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AN - SCOPUS:85210952025
SN - 0004-637X
VL - 977
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - 7
ER -