pith. sign in

arxiv: 2606.11378 · v1 · pith:ZZZJGXZVnew · submitted 2026-06-09 · 🌌 astro-ph.HE · astro-ph.GA

The Light Curve of Wind-Reprocessed Tidal Disruption Events

Brenna Mockler , David Khatami , Daniel Kasen , Xiaoshan Huang , Anthony L. Piro This is my paper

Pith reviewed 2026-06-27 11:52 UTC · model grok-4.3

classification 🌌 astro-ph.HE astro-ph.GA
keywords tidal disruption eventsreprocessingoutflowslight curvesX-ray emissionoptical emissionradiative transfer
0
0 comments X

The pith

The optical peak in tidal disruption events lags the bolometric peak by about three weeks due to reprocessing layer buildup.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

This paper models tidal disruption events by simulating a compact high-energy source surrounded by outflowing material that reprocesses radiation into longer wavelengths. The simulations track how the outflow accumulates over months and gradually obscures the central X-ray and EUV emission while producing optical and UV light. The optical/UV light curve follows a similar overall shape to the total energy output but reaches its maximum roughly three weeks later because the reprocessing layer needs time to develop sufficient optical depth. A reader would care because this delay means optical surveys alone can miss the earliest high-energy phase and underestimate when the star was first disrupted and when mass began returning to the black hole.

Core claim

Time-dependent 1D radiation hydrodynamic simulations of a compact evolving X-ray and EUV source with surrounding reprocessing outflow show that an early X-ray flare fades as material builds up and obscures the source, while the optical/UV luminosity rises and peaks about three weeks after the bolometric peak due to the time required to build the reprocessing layer.

What carries the argument

The time-dependent reprocessing outflow that accumulates optical depth around a central high-energy source, converting X-ray and EUV radiation into optical and UV emission on a wavelength-dependent timescale.

If this is right

  • Early high-energy emission from TDEs may be missed for events discovered in optical surveys.
  • The initial disruption and mass return time to the black hole may occur earlier than optical light curves suggest.
  • The efficiency of reprocessing changes with time in the evolving environment.
  • Key observables including timescales, luminosities, and color evolution are reproduced by the reprocessing mechanism.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • The offset implies that mass fallback rate estimates derived from optical data alone may need adjustment for the delayed peak.
  • Coordinated X-ray and optical monitoring from the first days after a disruption could directly test the predicted early flare and subsequent fade.
  • Similar buildup delays in reprocessing outflows could affect light-curve interpretations in other super-Eddington accretion systems.

Load-bearing premise

The simulations assume that luminosities and mass flow rates taken from prior hydrodynamical simulations of tidal disruptions, together with a compact central source surrounded by outflow, capture the dominant emission mechanism.

What would settle it

A well-observed tidal disruption event in which the optical and bolometric peaks occur simultaneously with no three-week offset, or one that shows no early X-ray flare before the optical rise.

Figures

Figures reproduced from arXiv: 2606.11378 by Anthony L. Piro, Brenna Mockler, Daniel Kasen, David Khatami, Xiaoshan Huang.

Figure 1
Figure 1. Figure 1: This cartoon depicts the main components of a wind-reprocessed TDE. In our simulation, we are assuming a hot X-ray source at the size scale of the forming disk, and reprocessing its emission through winds outflowing from the same radius. As this is a 1D simulation, we do not include the stream, however we use the orbital properties of the dis￾ruption to determine the circularization radius and mass and lum… view at source ↗
Figure 2
Figure 2. Figure 2: We simulate the rise, peak, and initial decay of a TDE using MCRT + 1D hydrodynamics. Top Plot: We plot the intrinsic optical/UV evolution, scaled to the peak luminosity in each banda . We find that higher energy bands peak earlier, and UV/optical emission peaks weeks after the bolometric luminosity. X-rays peak before the bolometric luminosity, then get absorbed by the growing outflow which in turn produc… view at source ↗
Figure 3
Figure 3. Figure 3: The blue, green, and orange lines show the output SED using 3 different opacity prescriptions – bound￾free (blue), bound-free + free-free (green), and bound-free + free-free + bound-bound (orange). All three also include electron scattering opacities. The top plot shows emission early on the rise at 7 days into the simulation, the middle plot shows emission at 49 days (near optical/UV peak), and the bottom… view at source ↗
Figure 4
Figure 4. Figure 4: Top: Fraction of oxygen in different ionization states as a function of radius at two representative times in the light curve. Opacities at radii denoted by rainbow vertical lines are plotted in bottom plots. Bottom: Opacity due to bound-free, free-free, and bound-bound transitions at various radii throughout outflows plotted at the same times as ionization states in top plots. Prominent ionization edges a… view at source ↗
Figure 5
Figure 5. Figure 5: Top: We find that adiabatic losses result in a peak luminosity that is ∼ 6× lower than the input luminosity (Lsource). Analytic predictions based on the evolving density profile in the simulations and Lsource predict a higher lumi￾nosity (smaller adiabatic losses, dashed line). However, these predictions assume that all adiabatic losses occur interior to rtrap (that all luminosity interior to Rtrap is adve… view at source ↗
Figure 6
Figure 6. Figure 6: Relevant hydro quantities as a function of time and radius from the fiducial simulation run. B. TREATMENT OF LINE ABSORPTION We find that when varying the value of of the line absorption parameter ϵ, the magnitude of the continuum emission does not vary significantly except in the extreme UV. We do see that the strength of the lines varies (as expected), but the continuum emission in the observable optical… view at source ↗
Figure 7
Figure 7. Figure 7: Here we compare the SED evolution for simulations with three different values of the line opacity ϵ parameter: 0.01, 0.1, and 0.3. 24 M˙ edd, comparable to the Eddington ratios in our simulation (for a 3 × 106M⊙ black hole). The peak fallback rate in our simulation is 26M˙ edd (assuming the canonical thin disk efficiency of 0.1), however at optical peak the fallback rate is 14M˙ edd. Given this, we compare… view at source ↗
Figure 8
Figure 8. Figure 8: We compare 3 epochs of our simulation with Sedona non-LTE post-processing results from Thomsen et al. (2022). We use a gaussian smoothing kernel to better compare with the lower resolution in Thomsen et al. (2022). 2.0 1.5 1.0 0.5 0.0 0.5 1.0 1.5 2.0 radius (cm) 0 1000 2000 3000 4000 radiation temperature (K) time = 3.33e-11s time = 7.33e-11s time = 1.13e-10s time = 1.53e-10s time = 1.93e-10s analytic diff… view at source ↗
Figure 9
Figure 9. Figure 9: The advected pulse problem solved analytically in the diffusion approximation (solid lines) and using Sedona (open circles). Andalman, Z. L., Quataert, E., Coughlin, E. R., & Nixon, C. J. 2025, Resolving the (Debate About) Nozzle Shocks in Tidal Disruption Events, arXiv, doi: 10.48550/arXiv.2512.08928 Aspegren, O., & Kasen, D. 2026, The Emission and Suppression of Line Features in Luminous Transients, arXi… view at source ↗
read the original abstract

The source of the optical/UV emission in tidal disruption events (TDEs) remains an enduring question in the field. Connecting the observed emission to the source is critical for both our understanding of these transients and for using TDEs to study the efficiency of super-Eddington accretion and black hole growth. To explore this connection, we ran time-dependent 1D radiation hydrodynamic simulations of TDE emission with the Sedona monte carlo radiative transfer code, focusing on the reprocessing paradigm. Our simulations follow a compact, evolving X-ray and EUV bright source and surrounding reprocessing outflow over multiple months, using luminosities and mass flow rates consistent with hydro simulations of tidal disruptions. We determine the efficiency of reprocessing as a function of time in this dramatically changing environment and reproduce key observables including timescales, luminosities, and color evolution. Notably, we see a strong wavelength-dependence in the emission timescale due to reprocessing effects. Early on there is an X-ray flare which quickly fades as material builds up and obscures the hot source. At the same time, the optical/UV luminosity begins to rise. Though the optical/UV light curve has a similar shape to the bolometric light curve, the optical peak is offset by $\sim$3 weeks from the bolometric peak due to the time required to build up the reprocessing layer. This implies that early time, high energy emission may be missed for TDEs discovered in optical surveys, and the initial disruption and mass return time to the black hole may occur earlier than optical light curves suggest.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

3 major / 2 minor

Summary. The manuscript presents time-dependent 1D radiation hydrodynamic simulations of wind-reprocessed tidal disruption events (TDEs) using the Sedona Monte Carlo code. Inputs for central luminosity and mass-flow rate Ṁ(t) are taken directly from prior non-radiative hydrodynamical TDE simulations. The simulations follow the evolution of a compact X-ray/EUV source surrounded by an outflow over months and report reproduction of observed timescales, luminosities, and color evolution. The central result is a wavelength-dependent emission timescale in which an early X-ray flare fades as the reprocessing layer builds up, while the optical/UV light curve peaks ~3 weeks after the bolometric peak due to the time required for sufficient column density to obscure the central source.

Significance. If the reported offset holds under the modeling assumptions, the work supplies a concrete physical mechanism linking the reprocessing outflow to the observed delay between high-energy and optical/UV peaks. This carries implications for the interpretation of optical-survey TDE samples and for the inferred timing of the initial disruption and mass return. The time-dependent treatment and direct comparison to multiple observables constitute a strength of the approach.

major comments (3)
  1. [Abstract] Abstract and Methods: the ~3-week optical/UV lag is produced by the accumulation of column in the outflow, but both the central luminosity history and Ṁ(t) are prescribed from earlier non-radiative hydrodynamical runs without radiation feedback onto the accretion rate. Because the radiative transfer and outflow dynamics are not coupled back to the central engine, the build-up timescale is not self-consistently determined and could shift if feedback were included.
  2. [Abstract] Abstract and Simulation Setup: the adopted 1D spherical geometry fixes the covering factor and the radial optical-depth evolution. This choice directly controls the wavelength-dependent obscuration timescale that produces the reported offset; the result may not generalize to bipolar or disk-wind geometries that are more commonly expected in TDEs.
  3. [Results] Results section: the manuscript states that the simulations reproduce key observables but supplies no error bars, convergence tests with respect to spatial or frequency resolution, or quantitative description of how the input Ṁ(t) and luminosity curves were selected or interpolated from the prior hydro runs. These omissions make it impossible to assess the robustness of the 3-week offset claim.
minor comments (2)
  1. [Abstract] The abstract introduces the Sedona code but does not state the dimensionality or the Monte Carlo specifics until later; a single sentence clarifying the numerical method at first mention would improve readability.
  2. Notation for the time-dependent mass-flow rate should be defined explicitly on first use rather than assumed from the cited hydro papers.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their constructive comments on our manuscript. We address each major point below, agreeing where the critique is valid and outlining specific revisions to improve clarity, robustness, and discussion of limitations.

read point-by-point responses

  1. Referee: [Abstract] Abstract and Methods: the ~3-week optical/UV lag is produced by the accumulation of column in the outflow, but both the central luminosity history and Ṁ(t) are prescribed from earlier non-radiative hydrodynamical runs without radiation feedback onto the accretion rate. Because the radiative transfer and outflow dynamics are not coupled back to the central engine, the build-up timescale is not self-consistently determined and could shift if feedback were included.

    Authors: We agree that prescribing luminosity and Ṁ(t) from non-radiative runs without feedback means the column build-up timescale is not fully self-consistent. This is a deliberate modeling choice to isolate reprocessing effects using existing hydro inputs, but we acknowledge it as a limitation. We will revise the Abstract and Methods to explicitly state the assumption of fixed inputs and add a paragraph discussing how radiation feedback could alter the offset. We will also note this in the context of the reported ~3-week lag. revision: partial

  2. Referee: [Abstract] Abstract and Simulation Setup: the adopted 1D spherical geometry fixes the covering factor and the radial optical-depth evolution. This choice directly controls the wavelength-dependent obscuration timescale that produces the reported offset; the result may not generalize to bipolar or disk-wind geometries that are more commonly expected in TDEs.

    Authors: The 1D spherical assumption does fix the covering factor and radial optical depth evolution, which directly influences the obscuration timescale. We selected this geometry to enable time-dependent Monte Carlo radiative transfer over months while remaining computationally feasible. We agree the result may differ in bipolar or disk-wind geometries. We will expand the Simulation Setup section to justify the 1D choice, quantify its impact on covering factor, and discuss how the offset might change in more realistic multi-dimensional configurations. revision: yes

  3. Referee: [Results] Results section: the manuscript states that the simulations reproduce key observables but supplies no error bars, convergence tests with respect to spatial or frequency resolution, or quantitative description of how the input Ṁ(t) and luminosity curves were selected or interpolated from the prior hydro runs. These omissions make it impossible to assess the robustness of the 3-week offset claim.

    Authors: We will add error bars to the reported light curves, provide a quantitative description of the interpolation procedure used for the input Ṁ(t) and luminosity histories from the prior hydrodynamical runs, and include convergence tests (or resolution justification) with respect to spatial and frequency grids. These additions will be placed in the Results and Methods sections to allow assessment of the robustness of the wavelength-dependent timescales. revision: yes

Circularity Check

0 steps flagged

No significant circularity; offset emerges from independent dynamical simulation.

full rationale

The paper's central result—the ~3-week optical/UV lag relative to the bolometric peak—is produced by the time-dependent build-up of column density in the 1D radiative transfer simulation. Inputs (luminosity history and Ṁ(t)) are taken from external prior hydrodynamical TDE simulations and are not fitted or defined in terms of the target observable. No equations reduce the output to the input by construction, no parameters are renamed as predictions, and no load-bearing self-citations or ansatzes are invoked. The derivation chain is self-contained and independent of the reported lag.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

Inputs drawn from prior hydro simulations; reprocessing paradigm treated as given framework; no new free parameters or invented entities introduced in the abstract.

axioms (1)
  • domain assumption Luminosities and mass flow rates are consistent with hydro simulations of tidal disruptions
    Directly used as boundary conditions for the radiation-hydro runs.

pith-pipeline@v0.9.1-grok · 5825 in / 1195 out tokens · 18534 ms · 2026-06-27T11:52:47.897023+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

300 extracted references · 1 linked inside Pith

  1. [1]

    arXiv:2202.10478 [astro-ph] , author =

    Light. arXiv:2202.10478 [astro-ph] , author =. 2022 , note =

    arXiv 2022

  2. [2]

    Monthly Notices of the Royal Astronomical Society , author =

    First light from tidal disruption events , volume =. Monthly Notices of the Royal Astronomical Society , author =. 2021 , note =. doi:10.1093/mnras/stab398 , abstract =

    doi:10.1093/mnras/stab398 2021

  3. [3]

    arXiv:2203.01461 [astro-ph] , author =

    The. arXiv:2203.01461 [astro-ph] , author =. 2022 , note =

    arXiv 2022

  4. [4]

    ApJL , author =

    The. ApJL , author =. 2022 , pages =. doi:10.3847/2041-8213/ac574b , abstract =

    doi:10.3847/2041-8213/ac574b 2022

  5. [5]

    arXiv:2203.06185 [astro-ph] , author =

    Across the. arXiv:2203.06185 [astro-ph] , author =. 2022 , note =

    arXiv 2022

  6. [6]

    Trujillo, I and Erwin, Peter and Ramos, A Asensio , year =

  7. [7]

    Rates of stellar tidal disruption as probes of the supermassive black hole mass function , abstract =

    Stone, Nicholas C and Metzger, Brian D , year =. Rates of stellar tidal disruption as probes of the supermassive black hole mass function , abstract =

  8. [8]

    ApJ , author =

    The. ApJ , author =. 2022 , pages =. doi:10.3847/1538-4357/ac480c , abstract =

    doi:10.3847/1538-4357/ac480c 2022

  9. [9]

    2021 , pages =

    The Astrophysical Journal , author =. 2021 , pages =

    2021

  10. [10]

    Monthly Notices of the Royal Astronomical Society , author =

    Tidal disruption events in post-starburst galaxies: the importance of a complete stellar mass function , volume =. Monthly Notices of the Royal Astronomical Society , author =. 2022 , note =. doi:10.1093/mnras/stac262 , abstract =

    doi:10.1093/mnras/stac262 2022

  11. [11]

    arXiv:2203.08162 [astro-ph] , author =

    Using the. arXiv:2203.08162 [astro-ph] , author =. 2022 , note =

    arXiv 2022

  12. [12]

    Monthly Notices of the Royal Astronomical Society , author =

    The merger rate of galaxies in the. Monthly Notices of the Royal Astronomical Society , author =. 2015 , note =. doi:10.1093/mnras/stv264 , abstract =

    doi:10.1093/mnras/stv264 2015

  13. [13]

    Astronomy and Astrophysics , author =

    The dominant role of mergers in the size evolution of massive early-type galaxies since z. Astronomy and Astrophysics , author =. 2012 , pages =. doi:10.1051/0004-6361/201219085 , abstract =

    doi:10.1051/0004-6361/201219085 2012

  14. [14]

    The Astrophysical Journal , author =

    The. The Astrophysical Journal , author =. 2009 , note =. doi:10.1088/0004-637X/697/2/1369 , abstract =

    doi:10.1088/0004-637x/697/2/1369 2009

  15. [15]

    Man, Allison W. S. and Toft, Sune and Zirm, Andrew W. and Wuyts, Stijn and Wel, Arjen van der , month = dec, year =. ApJ , publisher =. doi:10.1088/0004-637X/744/2/85 , abstract =

    doi:10.1088/0004-637x/744/2/85

  16. [16]

    Monthly Notices of the Royal Astronomical Society , author =

    A surprisingly high pair fraction for extremely massive galaxies at z. Monthly Notices of the Royal Astronomical Society , author =. 2009 , note =. doi:10.1111/j.1745-3933.2008.00608.x , abstract =

    doi:10.1111/j.1745-3933.2008.00608.x 2009

  17. [17]

    The Astrophysical Journal , author =

    The. The Astrophysical Journal , author =. 2012 , note =. doi:10.1088/0004-637X/747/1/34 , abstract =

    doi:10.1088/0004-637x/747/1/34 2012

  18. [18]

    arXiv:2201.02649 [astro-ph] , author =

    Systematic light curve modelling of. arXiv:2201.02649 [astro-ph] , author =. 2022 , note =

    arXiv 2022

  19. [19]

    New Astronomy , author =

    Resonant relaxation in stellar systems , volume =. New Astronomy , author =. 1996 , keywords =. doi:10.1016/S1384-1076(96)00012-7 , abstract =

    doi:10.1016/s1384-1076(96)00012-7 1996

  20. [20]

    The Astrophysical Journal , author =

    The. The Astrophysical Journal , author =. 1993 , note =. doi:10.1086/173366 , abstract =

    doi:10.1086/173366 1993

  21. [21]

    metallicities of the broad emission line regions in the nitrogen-loudest quasars

  22. [22]

    Monthly Notices of the Royal Astronomical Society: Letters , author =

    White dwarfs stripped by massive black holes: sources of coincident gravitational and electromagnetic radiation , volume =. Monthly Notices of the Royal Astronomical Society: Letters , author =. 2010 , pages =. doi:10.1111/j.1745-3933.2010.00930.x , abstract =

    doi:10.1111/j.1745-3933.2010.00930.x 2010

  23. [23]

    Monthly Notices of the Royal Astronomical Society , author =

    Tidal disruption by extreme mass ratio binaries and application to. Monthly Notices of the Royal Astronomical Society , author =. 2018 , note =. doi:10.1093/mnras/stx3039 , abstract =

    doi:10.1093/mnras/stx3039 2018

  24. [24]

    Monthly Notices of the Royal Astronomical Society , author =

    Tidal disruption events from supermassive black hole binaries , volume =. Monthly Notices of the Royal Astronomical Society , author =. 2017 , note =. doi:10.1093/mnras/stw2913 , abstract =

    doi:10.1093/mnras/stw2913 2017

  25. [25]

    The Astrophysical Journal , author =

    Triggering of. The Astrophysical Journal , author =. 1994 , note =. doi:10.1086/187299 , abstract =

    doi:10.1086/187299 1994

  26. [26]

    Astronomy and Astrophysics, v.371, p.806-815 (2001) , author =

    On faint companions in the close environment of star-forming dwarf galaxies. Astronomy and Astrophysics, v.371, p.806-815 (2001) , author =. 2001 , pages =. doi:10.1051/0004-6361:20010446 , abstract =

    doi:10.1051/0004-6361:20010446 2001

  27. [27]

    and Bournaud, F

    Renaud, F. and Bournaud, F. and Agertz, O. and Kraljic, K. and Schinnerer, E. and Bolatto, A. and Daddi, E. and Hughes, A. , month = may, year =. A diversity of starburst-triggering mechanisms in interacting galaxies and their signatures in. Astronomy & Astrophysics, Volume 625, id.A65,. doi:10.1051/0004-6361/201935222 , abstract =

    doi:10.1051/0004-6361/201935222

  28. [28]

    Monthly Notices of the Royal Astronomical Society , author =

    Plunging fireworks: why do infalling galaxies light up on the outskirts of clusters? , volume =. Monthly Notices of the Royal Astronomical Society , author =. 2012 , note =. doi:10.1111/j.1365-2966.2012.22059.x , abstract =

    doi:10.1111/j.1365-2966.2012.22059.x 2012

  29. [29]

    Monthly Notices of the Royal Astronomical Society , author =

    Double starbursts triggered by mergers in hierarchical clustering scenarios , volume =. Monthly Notices of the Royal Astronomical Society , author =. 2002 , pages =. doi:10.1046/j.1365-8711.2002.05385.x , abstract =

    doi:10.1046/j.1365-8711.2002.05385.x 2002

  30. [30]

    Dynamical

    Madigan, Ann-Marie and Halle, Andrew and Moody, Mackenzie and McCourt, Michael and Nixon, Chris and Wernke, Heather , month = feb, year =. Dynamical. ApJ , publisher =. doi:10.3847/1538-4357/aaa714 , abstract =

    doi:10.3847/1538-4357/aaa714

  31. [31]

    The Astrophysical Journal , author =

    Kinematic. The Astrophysical Journal , author =. 1989 , note =. doi:10.1086/167332 , abstract =

    doi:10.1086/167332 1989

  32. [32]

    The Astrophysical Journal , author =

    Tidal. The Astrophysical Journal , author =. 2019 , note =. doi:10.3847/1538-4357/ab43df , abstract =

    doi:10.3847/1538-4357/ab43df 2019

  33. [33]

    Monthly Notices of the Royal Astronomical Society , author =

    Tidal disruption discs formed and fed by stream-stream and stream-disc interactions in global. Monthly Notices of the Royal Astronomical Society , author =. 2022 , note =. doi:10.1093/mnras/stab3444 , abstract =

    doi:10.1093/mnras/stab3444 2022

  34. [34]

    2010 , note =

    Physical Review D , author =. 2010 , note =. doi:10.1103/PhysRevD.81.104014 , abstract =

    doi:10.1103/physrevd.81.104014 2010

  35. [35]

    The Astrophysical Journal , author =

    The. The Astrophysical Journal , author =. 2007 , note =. doi:10.1086/520497 , abstract =

    doi:10.1086/520497 2007

  36. [36]

    Monthly Notices of the Royal Astronomical Society , author =

    A numerical study of vector resonant relaxation , volume =. Monthly Notices of the Royal Astronomical Society , author =. 2015 , note =. doi:10.1093/mnras/stv057 , abstract =

    doi:10.1093/mnras/stv057 2015

  37. [37]

    Monthly Notices of the Royal Astronomical Society , author =

    Resonant relaxation and the warp of the stellar disc in the. Monthly Notices of the Royal Astronomical Society , author =. 2011 , note =. doi:10.1111/j.1365-2966.2010.17897.x , abstract =

    doi:10.1111/j.1365-2966.2010.17897.x 2011

  38. [38]

    Monthly Notices of the Royal Astronomical Society , author =

    Gas-driven massive black hole binaries: signatures in the. Monthly Notices of the Royal Astronomical Society , author =. 2011 , note =. doi:10.1111/j.1365-2966.2010.17782.x , abstract =

    doi:10.1111/j.1365-2966.2010.17782.x 2011

  39. [39]

    The Astronomical Journal , author =

    Secular perturbations of asteroids with high inclination and eccentricity , volume =. The Astronomical Journal , author =. 1962 , note =. doi:10.1086/108790 , abstract =

    doi:10.1086/108790 1962

  40. [40]

    Planetary and Space Science , author =

    The evolution of orbits of artificial satellites of planets under the action of gravitational perturbations of external bodies , volume =. Planetary and Space Science , author =. 1962 , pages =. doi:10.1016/0032-0633(62)90129-0 , language =

    doi:10.1016/0032-0633(62)90129-0 1962

  41. [41]

    Annual Review of Astronomy and Astrophysics , author =

    The. Annual Review of Astronomy and Astrophysics , author =. 2016 , pages =. doi:10.1146/annurev-astro-081915-023315 , abstract =

    doi:10.1146/annurev-astro-081915-023315 2016

  42. [42]

    and Dotti, Massimo and Lodato, Giuseppe and Izquierdo-Villalba, David , month = apr, year =

    Mazzolari, Giovanni and Bonetti, Matteo and Sesana, Alberto and Colombo, Riccardo M. and Dotti, Massimo and Lodato, Giuseppe and Izquierdo-Villalba, David , month = apr, year =. Extreme

  43. [43]

    The Astrophysical Journal , author =

    The. The Astrophysical Journal , author =. 2002 , note =. doi:10.1086/341002 , abstract =

    doi:10.1086/341002 2002

  44. [44]

    Monthly Notices of the Royal Astronomical Society , author =

    Massive black hole binary mergers in dynamical galactic environments , volume =. Monthly Notices of the Royal Astronomical Society , author =. 2017 , note =. doi:10.1093/mnras/stw2452 , abstract =

    doi:10.1093/mnras/stw2452 2017

  45. [45]

    The Astrophysical Journal , author =

    Efficient. The Astrophysical Journal , author =. 2011 , note =. doi:10.1088/0004-637X/732/2/89 , abstract =

    doi:10.1088/0004-637x/732/2/89 2011

  46. [46]

    The Astrophysical Journal , author =

    The. The Astrophysical Journal , author =. 2000 , note =. doi:10.1086/308300 , abstract =

    doi:10.1086/308300 2000

  47. [47]

    2021 , note =

    The Astrophysical Journal , author =. 2021 , note =. doi:10.3847/1538-4357/abe38d , abstract =

    doi:10.3847/1538-4357/abe38d 2021

  48. [48]

    Monthly Notices of the Royal Astronomical Society , author =

    The metallicities of the broad emission line regions in the nitrogen-loudest quasars , volume =. Monthly Notices of the Royal Astronomical Society , author =. 2014 , note =. doi:10.1093/mnras/stu007 , abstract =

    doi:10.1093/mnras/stu007 2014

  49. [49]

    The Astrophysical Journal , author =

    The. The Astrophysical Journal , author =. 2019 , note =. doi:10.3847/1538-4357/ab2711 , abstract =

    doi:10.3847/1538-4357/ab2711 2019

  50. [50]

    The Astrophysical Journal , author =

    Physics of. The Astrophysical Journal , author =. 2019 , note =. doi:10.3847/1538-4357/ab1f09 , abstract =

    doi:10.3847/1538-4357/ab1f09 2019

  51. [51]

    The Astrophysical Journal , author =

    Wind-reprocessed. The Astrophysical Journal , author =. 2020 , note =. doi:10.3847/1538-4357/ab83f6 , abstract =

    doi:10.3847/1538-4357/ab83f6 2020

  52. [52]

    Monthly Notices of the Royal Astronomical Society , author =

    Gravitational interactions of stars with supermassive black hole binaries -. Monthly Notices of the Royal Astronomical Society , author =. 2018 , note =. doi:10.1093/mnras/sty822 , abstract =

    doi:10.1093/mnras/sty822 2018

  53. [53]

    Li, Shuo and Liu, F. K. and Berczik, Peter and Spurzem, Rainer , month = jan, year =. ApJ , publisher =. doi:10.3847/1538-4357/834/2/195 , abstract =

    doi:10.3847/1538-4357/834/2/195

  54. [54]

    and Kozinsky, Boris and Rasio, Frederic A

    Ford, Eric B. and Kozinsky, Boris and Rasio, Frederic A. , month = may, year =. Secular. ApJ , publisher =. doi:10.1086/308815 , language =

    doi:10.1086/308815

  55. [55]

    Monthly Notices of the Royal Astronomical Society , author =

    The tidal disruption rate in dense galactic cusps containing a supermassive binary black hole , volume =. Monthly Notices of the Royal Astronomical Society , author =. 2005 , note =. doi:10.1111/j.1365-2966.2005.08843.x , abstract =

    doi:10.1111/j.1365-2966.2005.08843.x 2005

  56. [56]

    Nature , author =

    Hot. Nature , author =. 2011 , note =. doi:10.1038/nature10076 , abstract =

    doi:10.1038/nature10076 2011

  57. [57]

    The Astrophysical Journal , author =

    The. The Astrophysical Journal , author =. 2011 , note =. doi:10.1088/0004-637X/742/2/94 , abstract =

    doi:10.1088/0004-637x/742/2/94 2011

  58. [58]

    Monthly Notices of the Royal Astronomical Society , author =

    Secular dynamics in hierarchical three-body systems , volume =. Monthly Notices of the Royal Astronomical Society , author =. 2013 , note =. doi:10.1093/mnras/stt302 , abstract =

    doi:10.1093/mnras/stt302 2013

  59. [59]

    Physical Review D , author =

    Relativistic three-body effects in hierarchical triples , volume =. Physical Review D , author =. 2020 , note =. doi:10.1103/PhysRevD.102.064033 , abstract =

    doi:10.1103/physrevd.102.064033 2020

  60. [60]

    Monthly Notices of the Royal Astronomical Society , author =

    Timescales of. Monthly Notices of the Royal Astronomical Society , author =. 2015 , note =. doi:10.1093/mnras/stv1552 , abstract =

    doi:10.1093/mnras/stv1552 2015

  61. [61]

    Monthly Notices of the Royal Astronomical Society , author =

    The stationary points of the hierarchical three-body problem , volume =. Monthly Notices of the Royal Astronomical Society , author =. 2020 , note =. doi:10.1093/mnras/staa2602 , abstract =

    doi:10.1093/mnras/staa2602 2020

  62. [62]

    The Astrophysical Journal , author =

    Is. The Astrophysical Journal , author =. 2013 , note =. doi:10.1088/0004-637X/762/2/95 , abstract =

    doi:10.1088/0004-637x/762/2/95 2013

  63. [63]

    ApJ , author =

    Direct. ApJ , author =. 2019 , pages =. doi:10.3847/1538-4357/ab3e4a , abstract =

    doi:10.3847/1538-4357/ab3e4a 2019

  64. [64]

    2016 , pages =

    ApJ , author =. 2016 , pages =. doi:10.3847/0004-637X/828/2/77 , abstract =

    doi:10.3847/0004-637x/828/2/77 2016

  65. [65]

    Coleman and Hamilton, Douglas P

    Miller, M. Coleman and Hamilton, Douglas P. , month = sep, year =. Four-. ApJ , publisher =. doi:10.1086/341788 , language =

    doi:10.1086/341788

  66. [66]

    Liu, F. K. and Li, Shuo and Komossa, S. , month = apr, year =. A. ApJ , publisher =. doi:10.1088/0004-637X/786/2/103 , abstract =

    doi:10.1088/0004-637x/786/2/103

  67. [67]

    2013 , pages =

    ApJ , author =. 2013 , pages =. doi:10.1088/2041-8205/771/2/L28 , abstract =

    doi:10.1088/2041-8205/771/2/l28 2013

  68. [68]

    The Astrophysical Journal , author =

    The. The Astrophysical Journal , author =. 2018 , note =. doi:10.3847/1538-4357/aada47 , abstract =

    doi:10.3847/1538-4357/aada47 2018

  69. [69]

    Unveiling the hosts of parsec-scale massive black hole binaries: morphology and electromagnetic signatures , shorttitle =

    Izquierdo-Villalba, David and Sesana, Alberto and Colpi, Monica , month = jul, year =. Unveiling the hosts of parsec-scale massive black hole binaries: morphology and electromagnetic signatures , shorttitle =

  70. [70]

    The Astrophysical Journal , author =

    A. The Astrophysical Journal , author =. 2022 , note =. doi:10.3847/1538-4357/ac32de , abstract =

    doi:10.3847/1538-4357/ac32de 2022

  71. [71]

    Nature , author =

    A 17-billion-solar-mass black hole in a group galaxy with a diffuse core , volume =. Nature , author =. 2016 , note =. doi:10.1038/nature17197 , abstract =

    doi:10.1038/nature17197 2016

  72. [72]

    The Astrophysical Journal , author =

    A. The Astrophysical Journal , author =. 2021 , note =. doi:10.3847/1538-4357/ac0896 , abstract =

    doi:10.3847/1538-4357/ac0896 2021

  73. [73]

    Monthly Notices of the Royal Astronomical Society , author =

    Recoiled star clusters in the. Monthly Notices of the Royal Astronomical Society , author =. 2012 , note =. doi:10.1111/j.1365-2966.2011.20078.x , abstract =

    doi:10.1111/j.1365-2966.2011.20078.x 2012

  74. [74]

    The Astrophysical Journal , author =

    Galaxy. The Astrophysical Journal , author =. 2021 , note =. doi:10.3847/1538-4357/abdbb1 , abstract =

    doi:10.3847/1538-4357/abdbb1 2021

  75. [75]

    Astronomy and Astrophysics , author =

    Mergers trigger active galactic nuclei out to z ∼ 0.6 , volume =. Astronomy and Astrophysics , author =. 2020 , pages =. doi:10.1051/0004-6361/201937178 , abstract =

    doi:10.1051/0004-6361/201937178 2020

  76. [76]

    The Astrophysical Journal Supplement Series , author =

    A. The Astrophysical Journal Supplement Series , author =. 2008 , note =. doi:10.1086/524363 , abstract =

    doi:10.1086/524363 2008

  77. [77]

    Science , author =

    Rapid. Science , author =. 2007 , note =. doi:10.1126/science.1141858 , abstract =

    doi:10.1126/science.1141858 2007

  78. [78]

    New Astronomy Reviews , author =

    The quest for dual and binary supermassive black holes:. New Astronomy Reviews , author =. 2019 , note =. doi:10.1016/j.newar.2020.101525 , abstract =

    doi:10.1016/j.newar.2020.101525 2019

  79. [79]

    Monthly Notices of the Royal Astronomical Society , author =

    The bulge masses of. Monthly Notices of the Royal Astronomical Society , author =. 2022 , note =. doi:10.1093/mnras/stac1810 , abstract =

    doi:10.1093/mnras/stac1810 2022

  80. [80]

    Monthly Notices of the Royal Astronomical Society , author =

    Rapid eccentricity oscillations and the mergers of compact objects in hierarchical triples , volume =. Monthly Notices of the Royal Astronomical Society , author =. 2014 , note =. doi:10.1093/mnras/stu039 , abstract =

    doi:10.1093/mnras/stu039 2014

Showing first 80 references.