On the Role of Dynamical Cooling in the Dynamics of Circumbinary Disks

Wang, Haiyang; Bai, Xue-Ning; Lai, Dong

doi:10.3847/1538-4357/acac77

Cited by 10 publications

(4 citation statements)

References 62 publications

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“…Circumbinary disk-driven outspirals were first observed in Miranda et al (2017) and later confirmed by numerous other studies (e.g., Moody et al 2019;Muñoz et al 2019;Duffell et al 2020). Subsequent studies have found that binary orbital evolution depends on the disk and binary parameters, such as the disk aspect ratio h/r (Tiede et al 2020;Dittmann & Ryan 2022, 2024Penzlin et al 2022), the disk viscosity (Miranda et al 2017;Dittmann & Ryan 2022, 2024Franchini et al 2022;Penzlin et al 2022), the cooling timescale (Sudarshan et al 2022;Wang et al 2023aWang et al , 2023bFranchini et al 2024), and the binary eccentricity (Miranda et al 2017;D'Orazio & Duffell 2021;Siwek et al 2023a). Lai & Muñoz (2023) recently presented a review summarizing the outcomes of many of these studies.…”

Section: Introductionmentioning

confidence: 61%

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The Santa Barbara Binary−disk Code Comparison

Duffell,

Dittmann,

D’Orazio

et al. 2024

ApJ

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We have performed numerical calculations of a binary interacting with a gas disk, using 11 different numerical methods and a standard binary−disk setup. The goal of this study is to determine whether all codes agree on a numerically converged solution and to determine the necessary resolution for convergence and the number of binary orbits that must be computed to reach an agreed-upon relaxed state of the binary−disk system. We find that all codes can agree on a converged solution (depending on the diagnostic being measured). The zone spacing required for most codes to reach a converged measurement of the torques applied to the binary by the disk is roughly 1% of the binary separation in the vicinity of the binary components. For our disk model to reach a relaxed state, codes must be run for at least 200 binary orbits, corresponding to about a viscous time for our parameters, 0.2(a 2Ω B /ν) binary orbits, where ν is the kinematic viscosity. The largest discrepancies between codes resulted from the dimensionality of the setup (3D vs. 2D disks). We find good agreement in the total torque on the binary between codes, although the partition of this torque between the gravitational torque, orbital accretion torque, and spin accretion torque depends sensitively on the sink prescriptions employed. In agreement with previous studies, we find a modest difference in torques and accretion variability between 2D and 3D disk models. We find cavity precession rates to be appreciably faster in 3D than in 2D.

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Section: Introductionmentioning

confidence: 61%

“…The two appear to be causally linked, but the details depend on the disk and binary parameters. In some cases, disks that are stable and do not achieve an eccentric cavity morphology result in inward migration (Franchini et al 2022;Wang et al 2023b;Dittmann & Ryan 2024).…”

Section: The First 100 Orbitsmentioning

confidence: 99%

The Santa Barbara Binary−disk Code Comparison

Duffell,

Dittmann,

D’Orazio

et al. 2024

ApJ

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“…W see Figure 4). Lastly, we note that because the precession rate is dominated by the outward radial pull of the CBD, we expect our results to be comparatively insensitive to system uncertainties like the disk thermodynamics (unlike the other orbital elements; see, e.g., Tiede et al 2020;Dittmann & Ryan 2022;Wang et al 2023) or whether the binary is prograde or retrograde (Appendix B).…”

Section: Resultsmentioning

confidence: 95%

Disk-induced Binary Precession: Implications for Dynamics and Multimessenger Observations of Black Hole Binaries

Tiede,

D’Orazio,

Zwick

et al. 2024

ApJ

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Many studies have recently documented the orbital response of eccentric binaries accreting from thin circumbinary disks, characterizing the change in the binary semimajor axis and eccentricity. We extend these calculations to include the precession of the binary’s longitude of periapse induced by the circumbinary disk, and we characterize this precession continuously with binary eccentricity e b for equal mass components. This disk-induced apsidal precession is prograde with a weak dependence on the binary eccentricity when e b ≲ 0.4 and decreases approximately linearly for e b ≳ 0.4; yet at all e b binary precession is faster than the rates of change to the semimajor axis and eccentricity by an order of magnitude. We estimate that such precession effects are likely most important for subparsec separated binaries with masses ≲107 M ⊙, like LISA precursors. We find that accreting, equal-mass LISA binaries with M < 106 M ⊙ (and the most massive M ∼ 107 M ⊙ binaries out to z ∼ 3) may acquire a detectable phase offset due to the disk-induced precession. Moreover, disk-induced precession can compete with general relativistic precession in a vacuum, making it important for observer-dependent electromagnetic searches for accreting massive binaries—like Doppler boost and binary self-lensing models—after potentially only a few orbital periods.

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“…Furthermore, Huang & Yu (2022) explored the effect of cooling on the Rossby wave instability (RWI) in PPDs through linear analysis. Sudarshan et al (2022) and Wang et al (2023) initiated studies on how thermodynamics affects the accretion of binary systems using numerical simulations. In addition to the parameterized β −cooling method mentioned above, some studies adopt realistic terms for heating and cooling in the energy equation (Ziampras et al 2020(Ziampras et al , 2023.…”

Section: Introductionmentioning

confidence: 99%

The Dependence of the Structure of Planet-opened Gaps in Protoplanetary Disks on Radiative Cooling

Zhang,

Huang,

Dong

2024

ApJ

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Planets can excite density waves and open annular gas gaps in protoplanetary disks. The depth of gaps is influenced by the evolving angular momentum carried by density waves. While the impact of radiative cooling on the evolution of density waves has been studied, a quantitative correlation to connect gap depth with the cooling timescale is lacking. To address this knowledge gap, we employ the grid-based code Athena++ to simulate disk-planet interactions, treating cooling as a thermal relaxation process. We establish quantitative dependencies of steady-state gap depth (Equation 36) and width (Equation 41) on planetary mass, Shakura–Sunyaev viscosity, disk scale height, and thermal relaxation timescale (β). We confirm previous results that gap opening is the weakest when the thermal relaxation timescale is comparable to the local dynamical timescale. Significant variations in gap depth, up to an order of magnitude, are found with different β. In terms of width, a gap is at its narrowest around β = 1, approximately 10%–20% narrower compared to the isothermal case. When β ∼ 100, it can be ∼20% wider, and higher viscosity enhances this effect. We derive possible masses of the gas gap-opening planets in AS 209, HD 163296, MWC 480, and HL Tau, accounting for the uncertainties in the local thermal relaxation timescale.

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On the Role of Dynamical Cooling in the Dynamics of Circumbinary Disks

Cited by 10 publications

References 62 publications

The Santa Barbara Binary−disk Code Comparison

The Santa Barbara Binary−disk Code Comparison

Disk-induced Binary Precession: Implications for Dynamics and Multimessenger Observations of Black Hole Binaries

The Dependence of the Structure of Planet-opened Gaps in Protoplanetary Disks on Radiative Cooling

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