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A structure-aware tidal prescription for rapid binary population synthesis predicts equilibrium tides 1–2 orders of magnitude and dynamical tides up to 7 orders of magnitude stronger than standard prescriptions.

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2026-08-03 01:13 UTC pith:IMJL6JXM

load-bearing objection Solid, useful methods paper that brings modern tidal theory into COMPAS; the always-on IGW dissipation is a real caveat but not a deal-breaker for the methods contribution. the 4 major comments →

arxiv 2602.10187 v2 pith:IMJL6JXM submitted 2026-02-10 astro-ph.SR astro-ph.HEgr-qc

Modern tidal interaction models for rapid binary population synthesis: I. Methods

Veome Kapil , Ilya Mandel , Evgeni Grishin , Jim Fuller , Jeff Riley , Emanuele Berti This is my paper
classification astro-ph.SR astro-ph.HEgr-qc
keywords binary population synthesistidal dissipationtidal Love numberequilibrium tidesdynamical tidesinternal gravity wavesinertial wavesbinary circularization
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

The paper argues that the full frequency- and structure-dependence of tidal dissipation can be compressed into fast, closed-form expressions suitable for rapid binary population synthesis. Its central claim is that a few stellar-structure quantities—convective-envelope depth and density, convective-core radius, buoyancy frequency at radiative-convective boundaries—together with tidal frequency determine the dissipative tidal response, so the code can evolve millions of binaries with tidal physics faithful to detailed simulations. If true, previous population-synthesis studies have systematically underestimated tidal strength by one to seven orders of magnitude for exactly the stars that matter for binary circularization, synchronization, mass-transfer, and gravitational-wave source spins. The paper demonstrates order-of-magnitude agreement with detailed simulations across mechanisms, and shows that solar-type binaries can circularize at periods up to about 10 days while giant-branch binaries can circularize out to roughly 5000-day orbits—both far beyond what standard models achieve.

Core claim

The paper's central discovery is that tidal dissipation in binary population synthesis can be encoded in a frequency- and structure-dependent imaginary tidal Love number without sacrificing computational speed. For equilibrium tides, the model replaces a constant tidal-friction efficiency with a convective envelope of estimated density and a frequency-dependent turbulent viscosity. For dynamical tides from internal gravity waves, it uses an excitation factor derived from the stellar structure—scaling with the ninth power of the convective-core radius for convective-core stars, and with the buoyancy frequency at the radiative-convective boundary for radiative-core stars. For inertial waves, i

What carries the argument

The load-bearing object is the imaginary tidal Love number Im[k_l,n^m(ω_t)]—the dissipative part of a star's gravitational response to the tidal potential—which sets tidal power and torque, and therefore the rates of change of semi-major axis, eccentricity, and spin. The paper feeds this object with three closed-form channels: a constant-density convective envelope with a frequency-dependent turbulent viscosity for equilibrium tides; an E2 excitation factor times the 8/3 power of a dimensionless tidal frequency for internal gravity waves, with separate E2 factors for convective-core and radiative-core stars; and a frequency-averaged inertial-wave formula that turns on when the orbital freque

Load-bearing premise

The load-bearing premise is that internal gravity waves always dissipate fully at every radiative-convective boundary: the paper omits the wave-breaking condition and drops gravity-wave tides entirely for stars with more than two structural layers, so if real stars quench these waves at low amplitudes or long orbital periods, the claimed dynamical-tide enhancements of 1–7 orders of magnitude are systematically overestimated.

What would settle it

A census of circularization periods: the model predicts solar-type binaries circularize out to about 10-day orbits on the main sequence, while standard models predict almost none; a cluster sample showing circularization only below about 2–3 days would rule out the enhancement. Quantitatively, the model gives a tidal quality factor of about 8.8 × 10^9 for a Sun-like star at a 1-day tidal period, so any empirical measurement from heartbeat-star apsidal motion or hot-Jupiter decay that sits well above this would contradict the prescription's strength—the paper itself notes equilibrium tides can

Watch this falsifier — get emailed when new claim-graph text bears on it.

If this is right

  • Solar-type binaries in rapid synthesis will now circularize within their main-sequence lifetimes at initial periods up to about 10 days and eccentricities below about 0.6, where standard recipes predict essentially no tidal evolution.
  • Equilibrium tidal strength varies by 1–2 orders of magnitude over a star's lifetime as its convective envelope evolves, with a characteristic boost as the binary approaches synchronization.
  • For convective-core stars, tidal strength decays sharply as the core shrinks on the main sequence (roughly as (R_c/R*)^9), so mass-only excitation coefficients overestimate late-main-sequence dynamical tides.
  • Giant-branch and AGB binaries circularize at substantially larger orbital periods (about 5000 days) than older models imply (about 3000 days), narrowing but not closing the gap with observed circularization periods.
  • Because the same structure-dependent Love numbers describe tides in planet-host stars, predictions for hot-Jupiter orbital decay and exoplanet circularization can be re-derived without an arbitrary constant stellar quality factor.

Where Pith is reading between the lines

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

  • If the paper is right, the observed circularization of solar-type cluster binaries—which equilibrium-tide-only models cannot explain—may be accounted for by the newly strong dynamical tides, without invoking anomalously low tidal quality factors.
  • A testable extension is to implement the wave-breaking condition that the paper omits: switching off internal-gravity-wave tides above the critical orbital period would produce a sharp drop in circularization efficiency near a few days for solar-type stars, observable in cluster period–eccentricity distributions.
  • The same structure-dependent Love numbers carry over to exoplanet systems, so hot-Jupiter tidal decay and the ages of circularized planet-hosting stars could be re-derived with structure-aware tides instead of a fixed stellar quality factor.
  • If the enhancement survives, compact-object binaries inherit it: black-hole and neutron-star progenitors that circularize and synchronize earlier will arrive at compact-binary formation with different spins and separations, changing population predictions for gravitational-wave sources.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit.

Referee Report

4 major / 5 minor

Summary. The paper presents a fast, closed-form tidal dissipation prescription for the binary population synthesis code COMPAS. It models equilibrium tides through a frequency-dependent turbulent viscosity in convective envelopes, dynamical tides through internal gravity waves (IGWs) excited at convective-radiative boundaries, and inertial-wave (IW) dissipation in convective envelopes. The authors implement the prescriptions, validate them against a solar-type equilibrium-tide comparison and a Sun+hot-Jupiter dynamical-tide comparison, and evolve four representative binaries (0.3+0.3 Msun, 1+1 Msun, 2.5+2.5 Msun, 3+3 Msun) against the Z77/Hurley reference model. The central claim is that this simple model retains the dominant stellar-structure and frequency dependence of tidal dissipation, agrees with detailed simulations to within an order of magnitude, and predicts equilibrium and dynamical tidal strengths that can exceed commonly used prescriptions by 1-2 and 1-7 orders of magnitude, respectively.

Significance. If the claims hold, this would be a valuable contribution: it would give population synthesis a structure- and frequency-aware tidal module, bridging the gap between expensive MESA/STAREVOL-based tidal calculations and million-system binary population studies. The paper is transparent about its approximations and ships explicit equations and COMPAS integration, which is a strength. However, the headline quantitative claims are currently stronger than the evidence supports. The most load-bearing issue is the "always efficient" IGW dissipation assumption, which is internally inconsistent with the quoted critical-period criterion and directly controls the claimed 1-7 order-of-magnitude enhancement for radiative-core stars. The dynamical-tide validation in Appendix A.2 is also partly circular, and the high-eccentricity application of low-eccentricity secular equations needs quantitative justification. These issues are fixable, so the paper warrants a major revision rather than rejection.

major comments (4)
  1. [§2.2.2, §2.4, §3.2, Fig. 5] The assumption that IGW dissipation is "always efficient" contradicts the manuscript's own critical-period statement. §2.2.2 states that the critical orbital period for solar-type stars is about 3 days on the MS and decreases with evolution, and that this critical period "should always be lower than even the shortest period binaries we consider." The 1 Msun + 1 Msun example in §3.2 starts at P_orb=10 days. If P_orb > P_crit, the high-amplitude wave-breaking condition used to justify efficient IGW damping is not satisfied. Yet Fig. 5 shows IGW dissipation dominating the early evolution and the abstract generalizes the 1-7 order-of-magnitude dynamical-tide enhancement to low-mass MS and giant stars. This is a load-bearing internal inconsistency, not just a caveat. I request a period-resolved sensitivity test: for example, switch off IGW dissipation when P_orb exceeds the quoted P_crit, or
  2. [§3.2, Figs. 4-5, Abstract] The 6-7 orders-of-magnitude dynamical-tide enhancement is measured against a Z77 model that the authors themselves describe as "technically irrelevant" for radiative-core stars with convective envelopes. Comparing a new model to an inapplicable reference does not establish a physical enhancement; it only documents the difference between two different model domains. The abstract's "1-7 orders of magnitude stronger" statement therefore overstates the physical significance. I recommend reframing the comparison: either compare against a modern, applicable prescription (e.g., Goodman & Dickson 1998, Terquem et al. 1998, Ahuir et al. 2021, Esseldeurs et al. 2024) or clearly label the Z77 comparison as an inapplicable benchmark and report the actual enhancement relative to an applicable modern model.
  3. [Appendix A.2, Eq. (A3)] The dynamical-tide validation is circular in an important way. The spin evolution is fitted piecewise-linearly to Fig. 7 of Ahuir et al. (2021) via Eq. (A3), and the resulting Love numbers are then compared with Fig. 9 of the same paper. Since the tidal frequency entering Im[k] is determined by the fitted spin, this comparison largely confirms that the code can reproduce the input spin history, not that the dissipation model is independently predictive. This is especially problematic because the target spin evolution in Ahuir et al. is itself affected by tides. I request an independent validation: self-consistently evolve the spin with the proposed tidal model and compare the resulting tidal Love numbers and spin evolution, or use a different dataset/observable that does not rely on fitting the target's spin.
  4. [§2.4, Eqs. (11)-(13), §3.2, Fig. 4] The secular tidal equations are formally truncated at O(e^2), yet they are applied at e_ZAMS=0.5 in the headline 1 Msun + 1 Msun example and in the high-eccentricity grid points of Fig. 4. The implementation further drops the O(e^2) terms as a numerical stopgap when spins exceed pseudo-synchronization, which breaks angular-momentum conservation in that regime. The manuscript acknowledges the issue, but the e=0.5 cases are central to the paper's qualitative conclusions, and the top panel of Fig. 4 shows binaries becoming wider and more eccentric, a behavior that may be an artifact of the truncated equations. I request a quantitative assessment of this systematic error, for example by comparing with a calculation that retains higher-order e terms (or with a smaller-e control case) for at least one of the fiducial binaries.
minor comments (5)
  1. [Throughout] LaTeX encoding artifacts appear in Brunt-Väisälä and in several author names (e.g., "V¨ais¨al¨a"); please fix the source to render correctly.
  2. [§3.2, p. 14] The text says the semi-latus rectum a(1-e^2) "should remain constant" under angular momentum conservation, but when angular momentum is exchanged with stellar spins, the orbital angular momentum—and hence the semi-latus rectum—is not constant. The subsequent comparison actually shows a small decrease, consistent with spin angular momentum gain. Please rephrase to avoid this error.
  3. [§2.2.2] The phrase "the critical period should always be lower than even the shortest period binaries we consider" is ambiguous and, as written, undermines the immediately following assumption of always-efficient IGW dissipation. Please state explicitly the direction of the inequality and how it justifies (or fails to justify) the modeling choice.
  4. [Fig. 3] The paper acknowledges numerical artifacts after 0.6×10^10 yr in panels (c) and (d). Please consider masking or clearly marking these time ranges in the figure, since they are visually prominent and could be mistaken for physical features.
  5. [§3.1] The comparison to observed circularization periods for low-mass binaries is brief. Given that the paper's equilibrium-tide model still underpredicts empirical circularization periods, a more explicit statement about which ingredient (frequency dependence, PMS tides, or missing physics) is most likely responsible would help the reader.

Circularity Check

1 steps flagged

The dynamical-tide validation in Appendix A.2 is partly self-referential: the spin history is fitted from Ahuir et al. Fig. 7 before the Love numbers are compared with Fig. 9 of the same paper. The core tidal formulas themselves are not fitted to the headline claim.

specific steps
  1. fitted input called prediction [Appendix A.2, Eq. (A3), Fig. 11]
    "To reproduce their results, we must first obtain the spin evolution shown in Fig. 7 of J. Ahuir et al. (2021) so that we may correctly estimate the tidal period. As a simple fit to their plot, we construct the following piecewise linear model ... The results for IW and IGW tidal contributions are shown in Fig. 11, and should be compared against Fig. 9 of J. Ahuir et al. (2021). On the MS, our results agree very well with their 1M⊙ curve..."

    The fitted spin history Ω(t) from Eq. (A3) enters the tidal-frequency variable s_{n,m} = |nω_orb − mΩ_spin| (R_*^3/GM_*)^{1/2}, which controls the IGW Love number in Eq. (32) and sets the threshold for IW dissipation. The resulting dissipation curves are then compared against Fig. 9 of the same Ahuir et al. paper whose Fig. 7 supplied the spin input. Thus the frequency-dependent part of this 'agreement' is not an independent prediction of the dynamical-tide model but a consistency check that shares input data with the comparison target. The amplitude/structure part is still computed from COMPAS stellar models, so the circularity is partial and confined to this validation.

full rationale

The paper's central derivation is assembled from published external formalisms (Barker 2020; Duguid et al. 2020; Kushnir et al. 2017; Ogilvie 2013; Ahuir et al. 2021) and implemented in COMPAS; the Love-number expressions depend on stellar-structure quantities from COMPAS/Hurley fits rather than on the target outcomes. The main comparisons against Z77 are implementation comparisons and are not circular. The one genuinely self-referential step is Appendix A.2, where the spin evolution is fitted from Fig. 7 of Ahuir et al. and then used as an input to the tidal-frequency dependence before the result is compared with Fig. 9 of that same paper. This weakens that particular validation but does not infect the equilibrium-tide comparison, the Z77 comparisons, or the underlying formula derivations. The Shikauchi et al. core-radius fit in Eq. (30) is an external calibration to 1D stellar simulations despite author overlap, and the always-on IGW assumption is a modeling caveat rather than circular reasoning. Overall, the central results are substantially independent, with one partial self-referential validation.

Axiom & Free-Parameter Ledger

7 free parameters · 8 axioms · 0 invented entities

The paper introduces no new physical entities: all dissipation channels are existing theory. The central claim rests on a chain of simplified estimators for quantities COMPAS cannot compute directly (convective envelope density, mixing length, core radius, Brunt-Vaisala gradient), several of which are fitted to external stellar simulations or set by order-of-magnitude guesses. These estimators, not the underlying tidal formalism, carry most of the uncertainty.

free parameters (7)
  • ZAMS convective-core radius fit = 0.06 R_sun/M_sun, 0.05 R_sun/M_sun, 61.57 M_sun (Eq. 30)
    Convective-core radius at ZAMS is fit to 1D stellar simulations (Shikauchi et al. 2025); IGW tidal strength for convective-core stars scales steeply with core radius in Eqs. (26)-(29).
  • Density-contrast approximation for convective-core IGW tides = (rho_c/rho_bar)(1-rho_c/rho_bar)^2 ≈ 0.1
    Eq. (29) sets the prefactor by assuming rho_c/rho_bar ≈ 1/2; this order-of-magnitude choice sets the amplitude of convective-core IGW dissipation.
  • Beta_2,core = 1
    Eq. (29) sets beta_2,core=1 following Kushnir et al. (2017); changes the normalization of E_2,core.
  • Convective mixing-length estimate = l_c ≈ (R_* - R_conv)/2
    Eq. (24) approximates the mixing length as half the convective-envelope thickness. The authors note that overestimating l_c by a factor of 10 would overestimate viscous dissipation by about a factor of 5.
  • Brunt-Vaisala boundary approximations = N^2 ≈ GM_rad/R_conv^3; scale height H ≈ R_* - R_conv
    Eqs. (43)-(45) crudely estimate N^2 and d(N^2)/d ln r at the radiative-convective boundary; these feed directly into E_2,env in Eq. (35).
  • Density contrast gamma = rho_conv/rho_rad = derived from COMPAS stellar-type prescriptions
    Used in IW dissipation Eq. (46) and in E_2,env; depends on simplified Hurley/COMPAS envelope estimates rather than actual density profiles.
  • Spin-evolution fit for Ahuir comparison = piecewise linear Omega(t), t_0 = 4×10^7 yr (Eq. A3)
    Appendix A.2 fits the surface rotation history to Fig. 7 of Ahuir et al. (2021) before comparing tidal Love numbers to their Fig. 9; this is an auxiliary fit to the reference benchmark.
axioms (8)
  • domain assumption Tidal response is dominated by ℓ=2 multipole; higher multipoles are neglected.
    Sec. 2 after Eq. (10): “we will limit our expressions to only the ℓ=2 terms, which are dominant for tidal dissipation.â€
  • domain assumption Uniform stellar rotation and coplanar orbits; obliquity and differential rotation are ignored.
    Sec. 2.4 lists differential rotation as a major unmodelled effect; Sec. 2 says only coplanar orbits are considered.
  • ad hoc to paper Internal gravity wave dissipation is always efficient: wave breaking is always satisfied and IGWs are fully damped in radiative zones.
    Sec. 2.2.2: “we omit modeling the wave breaking condition for dynamical tides in our simulations, assuming instead that IGW dissipation is always efficient.†This is load-bearing for the dynamical-tide strength.
  • ad hoc to paper IGW dissipation is ignored in stars with more than two layers.
    Sec. 2.4: “we choose to ignore the contribution of IGW dissipation in stars with more than two layers,†assuming IGWs cannot propagate to efficient dissipation sites.
  • domain assumption Equilibrium tides arise only in convective envelopes; viscous dissipation in convective cores is neglected.
    Sec. 2.1: “we ignore the effects of viscous dissipation inside a convective core, assuming the core would be too small to meaningfully contribute.â€
  • ad hoc to paper The convective envelope can be treated as a constant-density shell with constant viscosity; Cowling approximation Phi+Psi ≈ Psi and g ≈ GM_*/r^2 hold near the surface.
    Between Eqs. (20) and (21), the authors use these approximations to evaluate the dissipation integral; they note the assumption is not valid in the deep interior or for deep convective envelopes.
  • ad hoc to paper Secular tidal equations truncated at O(e^2) are applied even at high eccentricity; O(e^2) terms are dropped as a numerical stopgap when spins exceed pseudo-synchronization.
    Sec. 2.4 states the equations are formally low-e only but no eccentricity limit is imposed; when the e^2 terms push spin beyond pseudo-synchronization, they are ignored.
  • domain assumption The Duguid et al. (2020) piecewise scaling of turbulent viscosity applies across all convective envelopes in the population-synthesis regime.
    Eq. (20) adopts this external scaling as the frequency-dependent viscosity; the central equilibrium-tide predictions inherit all its assumptions.

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In this work, we present an updated prescription of contemporary tidal dissipation theory adapted for rapid binary population synthesis. Our simplified expressions encode the dependence of tidal dissipation on stellar structure, stratification, and tidal forcing frequency, while remaining computationally efficient. We implement these prescriptions in the rapid population synthesis code COMPAS, and demonstrate the self-consistent coupling of tides with stellar evolution and binary properties such as orbital periods, spins, and eccentricities for several representative binary systems. When compared with commonly used tidal prescriptions, our equilibrium tidal dissipation efficiencies can be stronger by 1-2 orders of magnitude for low mass main sequence and giant type stars, and dynamical tides can be stronger by 1-7 orders of magnitude due to the explicit dependence on internal stellar structure and the presence of inertial wave dissipation. Despite our simplistic approach, our models agree with detailed stellar simulations to within an order of magnitude across tidal dissipation mechanisms.

Figures

Figures reproduced from arXiv: 2602.10187 by Emanuele Berti, Evgeni Grishin, Ilya Mandel, Jeff Riley, Jim Fuller, Veome Kapil.

Figure 1
Figure 1. Figure 1: Overview of tidal effects considered in this work, for stars with various internal structures. Convective envelopes may experience a combination of equilibrium tides from viscous dissipation, dynamical tides from internal gravity wave (IGW) dissipation, and dynamical tides from inertial wave (IW) dissipation. Boundaries between radiative and convective zones may excite dynamical tides from IGWs and IWs, wh… view at source ↗
Figure 2
Figure 2. Figure 2: Evolutionary tracks of e and Porb under equilib￾rium tides for 0.3M⊙ + 0.3M⊙ binaries, over a grid of initial orbital periods and initial eccentricities. Each binary is ini￾tialized on a grid in the Porb − e plane, and we plot the orbital period and eccentricity of each binary for every time step in COMPAS. The colors depict the age of each evolu￾tionary snapshot in years. The binaries are only evolved up … view at source ↗
Figure 3
Figure 3. Figure 3: Stellar and tidal evolution for a 0.3 M⊙ + 0.3 M⊙ binary with Porb,ZAMS = 2 days and eZAMS = 0.1. The binary is simulated for 14 Gyr, the approximate age of the Universe. lived 10−2 ≤ |ωt|/ωc ≤ 5 phase, finally settling into a stable (but noisy) phase once |ωt,22|/ωc ≤ 10−2 . Beyond this point, the effective viscosity no longer depends on ωt,22, and the Love number scales as ωt,22. Due to fi￾nite time-step… view at source ↗
Figure 4
Figure 4. Figure 4: Time evolution of e and Porb for 1M⊙ + 1M⊙ binaries over a grid of initial orbital periods and initial ec￾centricities, with our fiducial tides model (top panel) and the Z77 tides model (bottom panel). Each binary is initiated at a grid point, and the colors depict the age of each simulation snapshot in yr. The binaries are only evolved up to their MS lifetimes (approximately 10 Gyr) in this section. 3.2. … view at source ↗
Figure 5
Figure 5. Figure 5: Stellar and tidal evolution for a 1 M⊙ + 1 M⊙ binary with Porb,ZAMS=10 days and eZAMS = 0.5. The binary is simulated until the end of MS, at roughly 10 Gyr [PITH_FULL_IMAGE:figures/full_fig_p013_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Evolution of e under equilibrium tides for 2.5M⊙ + 2.5M⊙ binaries over a grid of initial orbital periods and initial eccentricities. The colors depict the age of each system in yr. The binaries are only evolved up to the end of their MS lifetimes, or until the binary merges, whichever comes first. 3.3. Convective core main sequence stars ZAMS stars above 1.25M⊙ have convective cores and radiative envelopes… view at source ↗
Figure 7
Figure 7. Figure 7: Stellar and tidal evolution for a 2.5 M⊙ + 2.5 M⊙ binary with Porb,ZAMS=3 days and eZAMS = 0.5. The binary is simulated until both MS stars merge at ∼ 420 Myr. observed circularization periods of AGB stellar binaries. The theoretical circularization period for stars that go through an AGB phase, such as the progenitors of Bar￾ium stars and WDs, has been estimated to be as large as ∼ 4000 days (O. Pols et a… view at source ↗
Figure 8
Figure 8. Figure 8: Evolution of e under equilibrium tides for 3M⊙ + 3M⊙ binaries over a grid of initial orbital periods and initial eccentricities. The colors represent the various stellar types encountered by each binary over its evolution. The binaries end in either stellar merger or as carbon-oxygen white dwarf (COWD) binaries at ∼ 450 Myr. a mechanism for circularized GB binaries to become ec￾centric (R. G. Izzard et al.… view at source ↗
Figure 9
Figure 9. Figure 9: Stellar and tidal evolution for a 3 M⊙ + 3 M⊙ binary with Porb,ZAMS=5000 days and eZAMS = 0.5. The binary is simulated until a WD+WD formation at ∼ 458 Myr. The dashed black lines show the boundaries between various stellar phases, and the phases are labeled above each plot [PITH_FULL_IMAGE:figures/full_fig_p018_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Strength of equilibrium tidal dissipation in our models as a function of the tidal frequency for a binary with initial mass M1,ZAMS = M2,ZAMS = 1M⊙, metallic￾ity Z = 0.02, and initial orbital period Porb,ZAMS = 1 day. The blue and red points are computed by plugging ν from Eq. (A1) and Eq. (A2) in Eq. (21), respectively. Each scatter point represents a time step in COMPAS. caused by our approximate expres… view at source ↗
Figure 11
Figure 11. Figure 11: Tidal dissipation through various channels for a Sun + Hot Jupiter binary system. The dotted line shows the equilibrium tidal dissipation in the convective zone (CZ), while the dashed and solid lines show the dynamical tide con￾tribution from inertial waves (convective zone) and internal gravity waves (radiative zone, RZ), respectively. simulations it tries to emulate, but may be much higher than empirica… view at source ↗

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  1. Modern tidal interaction models for rapid binary population synthesis: II. Binary black hole formation, mergers, and spins

    astro-ph.HE 2026-06 unverdicted novelty 4.0

    Simulations with a new tidal model in COMPAS predict that merging binary black holes from isolated evolution are strongly biased to low effective spins, with one third below 0.05 and only 3% above 0.5, but the high-sp...

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Works this paper leans on

79 extracted references · 4 canonical work pages · cited by 1 Pith paper

  1. [1]

    , " * write output.state after.block = add.period write newline

    ENTRY address archivePrefix author booktitle chapter doi edition editor eprint howpublished institution journal key month number organization pages publisher school series title misctitle type volume year version url label extra.label sort.label short.list INTEGERS output.state before.all mid.sentence after.sentence after.block FUNCTION init.state.consts ...

  2. [2]

    write newline

    " write newline "" before.all 'output.state := FUNCTION format.url url empty "" new.block "" url * "" * if FUNCTION format.eprint eprint empty "" archivePrefix empty "" archivePrefix "arXiv" = new.block " " eprint * " " * new.block " " eprint * " " * if if if FUNCTION format.doi doi empty "" " " doi * " " * if FUNCTION format.pid doi empty eprint empty ur...

  3. [3]

    """F ?OIV[o nƍMFG.>g

    thebibliography [1] 20pt to REFERENCES 6pt =0pt \@twocolumntrue 12pt -12pt 10pt plus 3pt =0pt =0pt =1pt plus 1pt =0pt =0pt -12pt =13pt plus 1pt =20pt =13pt plus 1pt \@M =10000 =-1.0em =0pt =0pt 0pt =0pt =1.0em @enumiv\@empty 10000 10000 `\.\@m \@noitemerr \@latex@warning Empty `thebibliography' environment \@ifnextchar \@reference \@latexerr Missing key o...

    arXiv 2017

  4. [4]

    P., et al

    Abbott, B. P., et al. 2019, title GWTC-1: A Gravitational-Wave Transient Catalog of Compact Binary Mergers Observed by LIGO and Virgo during the First and Second Observing Runs , Phys. Rev. X, 9, 031040, 10.1103/PhysRevX.9.031040

    doi:10.1103/physrevx.9.031040 2019

  5. [5]

    2021, title GWTC-2: Compact Binary Coalescences Observed by LIGO and Virgo During the First Half of the Third Observing Run , Phys

    Abbott, R., et al. 2021, title GWTC-2: Compact Binary Coalescences Observed by LIGO and Virgo During the First Half of the Third Observing Run , Phys. Rev. X, 11, 021053, 10.1103/PhysRevX.11.021053

    doi:10.1103/physrevx.11.021053 2021

  6. [6]

    2023, title GWTC-3: Compact Binary Coalescences Observed by LIGO and Virgo during the Second Part of the Third Observing Run , Phys

    Abbott, R., et al. 2023, title GWTC-3: Compact Binary Coalescences Observed by LIGO and Virgo during the Second Part of the Third Observing Run , Phys. Rev. X, 13, 041039, 10.1103/PhysRevX.13.041039

    doi:10.1103/physrevx.13.041039 2023

  7. [7]

    2021, title Dynamical tide in stellar radiative zones - General formalism and evolution for low-mass stars, Astronomy and Astrophysics, 651, A3, 10.1051/0004-6361/202040174

    Ahuir, J., Mathis, S., & Amard, L. 2021, title Dynamical tide in stellar radiative zones - General formalism and evolution for low-mass stars, Astronomy and Astrophysics, 651, A3, 10.1051/0004-6361/202040174

    doi:10.1051/0004-6361/202040174 2021

  8. [8]

    A., Sucerquia , M., Zuluaga , J

    Alvarado-Montes , J. A., Sucerquia , M., Zuluaga , J. I., & Schwab , C. 2025, title Orbital Decay of the Ultra-hot Jupiter TOI-2109b: Tidal Constraints and Transit-timing Analysis , Astrophys. J., 988, 66, 10.3847/1538-4357/ade057

    doi:10.3847/1538-4357/ade057 2025

  9. [9]

    Amard, L., Palacios, A., Charbonnel, C., et al. 2019, title First grids of low-mass stellar models and isochrones with self-consistent treatment of rotation-From 0.2 to 1.5 M⊙ at seven metallicities from PMS to TAMS, Astronomy & Astrophysics, 631, A77

    2019

  10. [10]

    Barker , A. J. 2020, title Tidal dissipation in evolving low-mass and solar-type stars with predictions for planetary orbital decay , Monthly Notices of the Royal Astronomical Society, 498, 2270, 10.1093/mnras/staa2405

    doi:10.1093/mnras/staa2405 2020

  11. [11]

    Barker, A. J. 2022, title Tidal dissipation due to inertial waves can explain the circularization periods of solar-type binaries, The Astrophysical Journal Letters, 927, L36

    2022

  12. [12]

    J., & Ogilvie, G

    Barker, A. J., & Ogilvie, G. I. 2010, title On internal wave breaking and tidal dissipation near the centre of a solar-type star , Mon. Not. Roy. Astron. Soc., 404, 1849, 10.1111/j.1365-2966.2010.16400.x

    arXiv 2010

  13. [13]

    S., Fragos, T., Qin, Y., et al

    Bavera, S. S., Fragos, T., Qin, Y., et al. 2020, title The origin of spin in binary black holes: Predicting the distributions of the main observables of Advanced LIGO , Astron. Astrophys., 635, A97, 10.1051/0004-6361/201936204

    doi:10.1051/0004-6361/201936204 2020

  14. [14]

    B., Cenko, A

    Behr, B. B., Cenko, A. T., Hajian, A. R., et al. 2011, title STELLAR ASTROPHYSICS WITH A DISPERSED FOURIER TRANSFORM SPECTROGRAPH. II. ORBITS OF DOUBLE-LINED SPECTROSCOPIC BINARIES, The Astronomical Journal, 142, 6, 10.1088/0004-6256/142/1/6

    doi:10.1088/0004-6256/142/1/6 2011

  15. [15]

    A., et al

    Belczynski, K., Kalogera, V., Rasio, F. A., et al. 2008, title Compact object modeling with the startrack population synthesis code , Astrophys. J. Suppl., 174, 223, 10.1086/521026

    doi:10.1086/521026 2008

  16. [16]

    2016, title New spectroscopic binary companions of giant stars and updated metallicity distribution for binary systems, Astronomy & Astrophysics, 593, A133

    Bluhm, P., Jones, M., Vanzi, L., et al. 2016, title New spectroscopic binary companions of giant stars and updated metallicity distribution for binary systems, Astronomy & Astrophysics, 593, A133

    2016

  17. [17]

    Brown, A. G. A., et al. 2018, title Gaia Data Release 2 : Summary of the contents and survey properties , Astron. Astrophys., 616, A1, 10.1051/0004-6361/201833051

    doi:10.1051/0004-6361/201833051 2018

  18. [18]

    1997, title Structure and evolution of low-mass stars , Astron

    Chabrier, G., & Baraffe, I. 1997, title Structure and evolution of low-mass stars , Astron. Astrophys., 327, 1039. astro-ph/9704118

    Pith/arXiv arXiv 1997

  19. [19]

    1997, title Circularization and synchronization times in Main-Sequence of detached eclipsing binaries II

    Claret, A., & Cunha, N. 1997, title Circularization and synchronization times in Main-Sequence of detached eclipsing binaries II. Using the formalisms by Zahn., Astronomy and Astrophysics, v. 318, p. 187-197, 318, 187

    1997

  20. [20]

    I., & Johnson, J

    Dawson, R. I., & Johnson, J. A. 2018, title Origins of hot Jupiters, Annual Review of Astronomy and Astrophysics, 56, 175

    2018

  21. [21]

    W., & Lai, D

    Dewberry, J. W., & Lai, D. 2022, title Dynamical Tidal Love Numbers of Rapidly Rotating Planets and Stars, The Astrophysical Journal, 925, 124, 10.3847/1538-4357/ac3ede

    doi:10.3847/1538-4357/ac3ede 2022

  22. [22]

    D., Barker, A

    Duguid, C. D., Barker, A. J., & Jones, C. A. 2020, title Convective turbulent viscosity acting on equilibrium tidal flows: new frequency scaling of the effective viscosity , Monthly Notices of the Royal Astronomical Society, 497, 3400, 10.1093/mnras/staa2216

    doi:10.1093/mnras/staa2216 2020

  23. [23]

    2024, title Gaia s binary star renaissance , New Astron

    El-Badry, K. 2024, title Gaia s binary star renaissance , New Astron. Rev., 98, 101694, 10.1016/j.newar.2024.101694

    arXiv 2024

  24. [24]

    2024, title Tidal dissipation in evolved low- and intermediate-mass stars , Astron

    Esseldeurs , M., Mathis , S., & Decin , L. 2024, title Tidal dissipation in evolved low- and intermediate-mass stars , Astron. Astrophys., 690, A266, 10.1051/0004-6361/202449648

    doi:10.1051/0004-6361/202449648 2024

  25. [25]

    2023, title POSYDON: A General-purpose Population Synthesis Code with Detailed Binary-evolution Simulations , Astrophys

    Fragos, T., et al. 2023, title POSYDON: A General-purpose Population Synthesis Code with Detailed Binary-evolution Simulations , Astrophys. J. Suppl., 264, 45, 10.3847/1538-4365/ac90c1

    doi:10.3847/1538-4365/ac90c1 2023

  26. [26]

    2017, title Heartbeat Stars, Tidally Excited Oscillations, and Resonance Locking , Mon

    Fuller, J. 2017, title Heartbeat Stars, Tidally Excited Oscillations, and Resonance Locking , Mon. Not. Roy. Astron. Soc., 472, 1538, 10.1093/mnras/stx2135

    doi:10.1093/mnras/stx2135 2017

  27. [27]

    M., Mathieu, R

    Geller, A. M., Mathieu, R. D., Latham, D. W., et al. 2021, title Stellar Radial Velocities in the Old Open Cluster M67 (NGC 2682). II. The Spectroscopic Binary Population, The Astronomical Journal, 161, 190

    2021

  28. [28]

    2018, title Spin orientations of merging black holes formed from the evolution of stellar binaries , Phys

    Gerosa, D., Berti, E., O'Shaughnessy, R., et al. 2018, title Spin orientations of merging black holes formed from the evolution of stellar binaries , Phys. Rev. D, 98, 084036, 10.1103/PhysRevD.98.084036

    doi:10.1103/physrevd.98.084036 2018

  29. [29]

    2013, title Resonant-plane locking and spin alignment in stellar-mass black-hole binaries: a diagnostic of compact-binary formation , Phys

    Gerosa, D., Kesden, M., Berti, E., O'Shaughnessy, R., & Sperhake, U. 2013, title Resonant-plane locking and spin alignment in stellar-mass black-hole binaries: a diagnostic of compact-binary formation , Phys. Rev. D, 87, 104028, 10.1103/PhysRevD.87.104028

    doi:10.1103/physrevd.87.104028 2013

  30. [30]

    Goldreich, P., & Nicholson, P. D. 1977, title Turbulent viscosity and Jupiter's tidal Q, Icarus, 30, 301

    1977

  31. [31]

    Goodman, J., & Dickson, E. S. 1998, title Dynamical tide in solar-type binaries , Astrophys. J., 507, 938, 10.1086/306348

    doi:10.1086/306348 1998

  32. [32]

    Grishin, E., & Perets, H. B. 2022, title Chaotic dynamics of wide triples induced by galactic tides: a novel channel for producing compact binaries, mergers, and collisions , Mon. Not. Roy. Astron. Soc., 512, 4993, 10.1093/mnras/stac706

    doi:10.1093/mnras/stac706 2022

  33. [33]

    2018, title KIC 8164262: a heartbeat star showing tidally induced pulsations with resonant locking, Monthly Notices of the Royal Astronomical Society, 473, 5165

    Hambleton, K., Fuller, J., Thompson, S., et al. 2018, title KIC 8164262: a heartbeat star showing tidally induced pulsations with resonant locking, Monthly Notices of the Royal Astronomical Society, 473, 5165

    2018

  34. [34]

    2010, title Calibration of Equilibrium Tide Theory for Extrasolar Planet Systems , Astrophys

    Hansen, B. 2010, title Calibration of Equilibrium Tide Theory for Extrasolar Planet Systems , Astrophys. J., 723, 285, 10.1088/0004-637X/723/1/285

    doi:10.1088/0004-637x/723/1/285 2010

  35. [35]

    R., Pols, O

    Hurley, J. R., Pols, O. R., & Tout, C. A. 2000, title Comprehensive analytic formulae for stellar evolution as a function of mass and metallicity , Mon. Not. Roy. Astron. Soc., 315, 543, 10.1046/j.1365-8711.2000.03426.x

    arXiv 2000

  36. [36]

    R., Tout, C

    Hurley, J. R., Tout, C. A., & Pols, O. R. 2002, title Evolution of binary stars and the effect of tides on binary populations , Mon. Not. Roy. Astron. Soc., 329, 897, 10.1046/j.1365-8711.2002.05038.x

    arXiv 2002

  37. [37]

    1981, title Tidal evolution in close binary systems., Astronomy and Astrophysics, 99, 126

    Hut, P. 1981, title Tidal evolution in close binary systems., Astronomy and Astrophysics, 99, 126. https://ui.adsabs.harvard.edu/abs/1981A&A....99..126H/abstract

    1981

  38. [38]

    Idini, B., & Stevenson, D. J. 2021, title Dynamical Tides in Jupiter as Revealed by Juno, The Planetary Science Journal, 2, 69, 10.3847/PSJ/abe715

    work page doi:10.3847/psj/abe715 2021

  39. [39]

    G., Dermine, T., & Church, R

    Izzard, R. G., Dermine, T., & Church, R. P. 2010, title White-Dwarf Kicks and Implications for Barium Stars , Astron. Astrophys., 523, A10, 10.1051/0004-6361/201015254

    doi:10.1051/0004-6361/201015254 2010

  40. [40]

    Kumar, P., & Quataert, E. J. 1997, title Differential rotation enhanced dissipation of tides in the psr j0045-7319 binary , Astrophys. J. Lett., 479, L51, 10.1086/310573

    work page doi:10.1086/310573 1997

  41. [41]

    A., & Waldman, R

    Kushnir, D., Zaldarriaga, M., Kollmeier, J. A., & Waldman, R. 2017, title Dynamical tides reexpressed , Monthly Notices of the Royal Astronomical Society, 467, 2146, 10.1093/mnras/stx255

    doi:10.1093/mnras/stx255 2017

  42. [42]

    M., Rappaport, S

    Levine, A. M., Rappaport, S. A., & Zojcheski, G. 2000, title Orbital decay in lmc x-4 , Astrophys. J., 541, 194, 10.1086/309398

    doi:10.1086/309398 2000

  43. [43]

    Love, A. E. H. 1909, title The yielding of the Earth to disturbing forces , Monthly Notices of the Royal Astronomical Society, 69, 476, 10.1093/mnras/69.6.476

    doi:10.1093/mnras/69.6.476 1909

  44. [44]

    2015, title Variation of tidal dissipation in the convective envelope of low-mass stars along their evolution, Astronomy & Astrophysics, 580, L3

    Mathis, S. 2015, title Variation of tidal dissipation in the convective envelope of low-mass stars along their evolution, Astronomy & Astrophysics, 580, L3

    2015

  45. [45]

    Maxted , P. F. L., Triaud , A. H. M. J., & Martin , D. V. 2023, title The EBLM Project From False Positives to Benchmark Stars and Circumbinary Exoplanets , Universe, 9, 498, 10.3390/universe9120498

    work page doi:10.3390/universe9120498 2023

  46. [46]

    Meibom, S., & Mathieu, R. D. 2005, title A Robust Measure of Tidal Circularization in Coeval Binary Populations: The Solar-Type Spectroscopic Binary Population in the Open Cluster M35*, The Astrophysical Journal, 620, 970, 10.1086/427082

    doi:10.1086/427082 2005

  47. [47]

    M., Hendriks, D

    Mirouh, G. M., Hendriks, D. D., Dykes, S., Moe, M., & Izzard, R. G. 2023, title Detailed equilibrium and dynamical tides: impact on circularization and synchronization in open clusters, Monthly Notices of the Royal Astronomical Society, 524, 3978, 10.1093/mnras/stad2048

    doi:10.1093/mnras/stad2048 2023

  48. [48]

    2017, title Mind Your Ps and Qs: The Interrelation between Period (P) and Mass-ratio (Q) Distributions of Binary Stars , Astrophys

    Moe, M., & Di Stefano, R. 2017, title Mind Your Ps and Qs: The Interrelation between Period (P) and Mass-ratio (Q) Distributions of Binary Stars , Astrophys. J. Suppl., 230, 15, 10.3847/1538-4365/aa6fb6

    doi:10.3847/1538-4365/aa6fb6 2017

  49. [49]

    Moe , M., & Kratter , K. M. 2018, title Dynamical Formation of Close Binaries during the Pre-main-sequence Phase , Astrophys. J., 854, 44, 10.3847/1538-4357/aaa6d2

    doi:10.3847/1538-4357/aaa6d2 2018

  50. [50]

    Ogilvie, G. I. 2013, title Tides in rotating barotropic fluid bodies: the contribution of inertial waves and the role of internal structure , Mon. Not. Roy. Astron. Soc., 429, 613, 10.1093/mnras/sts362

    doi:10.1093/mnras/sts362 2013

  51. [51]

    Ogilvie, G. I. 2014, title Tidal dissipation in stars and giant planets , Ann. Rev. Astron. Astrophys., 52, 171, 10.1146/annurev-astro-081913-035941

    doi:10.1146/annurev-astro-081913-035941 2014

  52. [52]

    I., & Lin, D

    Ogilvie, G. I., & Lin, D. N. C. 2007, title Tidal dissipation in rotating solar-type stars , Astrophys. J., 661, 1180, 10.1086/515435

    doi:10.1086/515435 2007

  53. [53]

    2011, title Modules for Experiments in Stellar Astrophysics (MESA) , Astrophys

    Paxton, B., Bildsten, L., Dotter, A., et al. 2011, title Modules for Experiments in Stellar Astrophysics (MESA) , Astrophys. J. Suppl., 192, 3, 10.1088/0067-0049/192/1/3

    doi:10.1088/0067-0049/192/1/3 2011

  54. [54]

    2013, title Modules for Experiments in Stellar Astrophysics (MESA): Planets, Oscillations, Rotation, and Massive Stars , Astrophys

    Paxton, B., et al. 2013, title Modules for Experiments in Stellar Astrophysics (MESA): Planets, Oscillations, Rotation, and Massive Stars , Astrophys. J. Suppl., 208, 4, 10.1088/0067-0049/208/1/4

    doi:10.1088/0067-0049/208/1/4 2013

  55. [55]

    Peale, S. J. 1999, title Origin and evolution of the natural satellites , Ann. Rev. Astron. Astrophys., 37, 533, 10.1146/annurev.astro.37.1.533

    work page doi:10.1146/annurev.astro.37.1.533 1999

  56. [56]

    G., Winn, J

    Penev, K., Bouma, L. G., Winn, J. N., & Hartman, J. D. 2018, title Empirical Tidal Dissipation in Exoplanet Hosts From Tidal Spin-up, The Astronomical Journal, 155, 165, 10.3847/1538-3881/aaaf71

    doi:10.3847/1538-3881/aaaf71 2018

  57. [57]

    2011, title Tidal Evolution of Close-in Extrasolar Planets: High Stellar Q from New Theoretical Models , Astrophys

    Penev, K., & Sasselov, D. 2011, title Tidal Evolution of Close-in Extrasolar Planets: High Stellar Q from New Theoretical Models , Astrophys. J., 731, 67, 10.1088/0004-637X/731/1/67

    doi:10.1088/0004-637x/731/1/67 2011

  58. [58]

    2024, title Fits for the convective envelope mass in massive stars , 2402.13180

    Picker, L., Hirai, R., & Mandel, I. 2024, title Fits for the convective envelope mass in massive stars , 2402.13180

    Pith/arXiv arXiv 2024

  59. [59]

    2003, title Can Standard Evolution Models Explain the Properties of Barium Stars? in Symbiotic Stars Probing Stellar Evolution, Vol

    Pols, O., Karakas, A., Lattanzio, J., & Tout, C. 2003, title Can Standard Evolution Models Explain the Properties of Barium Stars? in Symbiotic Stars Probing Stellar Evolution, Vol. 303, 290

    2003

  60. [60]

    2000, title Resolved double-lined spectroscopic binaries: A neglected source of hypothesis-free parallaxes and stellar masses, Astron

    Pourbaix, D. 2000, title Resolved double-lined spectroscopic binaries: A neglected source of hypothesis-free parallaxes and stellar masses, Astron. Astrophys. Sup., 145, 215, 10.1051/aas:2000237

    doi:10.1051/aas:2000237 2000

  61. [61]

    H., & Teukolsky , S

    Press , W. H., & Teukolsky , S. A. 1977, title On formation of close binaries by two-body tidal capture. , Astrophys. J., 213, 183, 10.1086/155143

    doi:10.1086/155143 1977

  62. [62]

    1961, title Vitesses radiales et \'e l \'e ments orbitaux de zeta1 Ursae Majoris, Journal des Observateurs, Vol

    Prevot, L. 1961, title Vitesses radiales et \'e l \'e ments orbitaux de zeta1 Ursae Majoris, Journal des Observateurs, Vol. 44, p. 83, 44, 83

    1961

  63. [63]

    2018, title The spin of the second-born black hole in coalescing binary black holes , Astron

    Qin, Y., Fragos, T., Meynet, G., et al. 2018, title The spin of the second-born black hole in coalescing binary black holes , Astron. Astrophys., 616, A28, 10.1051/0004-6361/201832839

    doi:10.1051/0004-6361/201832839 2018

  64. [64]

    A., Henry, T

    Raghavan, D., McAlister, H. A., Henry, T. J., et al. 2010, title A survey of stellar families: multiplicity of solar-type stars, The Astrophysical Journal Supplement Series, 190, 1

    2010

  65. [65]

    2024, title Dynamical tides in binaries: Inconsistencies in the implementation of Zahn s prescription , Astron

    Sciarini, L., Ekstr\"om, S., Eggenberger, P., et al. 2024, title Dynamical tides in binaries: Inconsistencies in the implementation of Zahn s prescription , Astron. Astrophys., 681, L1, 10.1051/0004-6361/202348424

    doi:10.1051/0004-6361/202348424 2024

  66. [66]

    2025, title Evolution of the Convective Core Mass during the Main Sequence , Astrophys

    Shikauchi, M., Hirai, R., & Mandel, I. 2025, title Evolution of the Convective Core Mass during the Main Sequence , Astrophys. J., 984, 149, 10.3847/1538-4357/adc5fa

    doi:10.3847/1538-4357/adc5fa 2025

  67. [67]

    2000, title An internet server for update pre-main sequence tracks of low- and intermediate-mass stars , Astron

    Siess, L., Dufour, E., & Forestini, M. 2000, title An internet server for update pre-main sequence tracks of low- and intermediate-mass stars , Astron. Astrophys., 358, 593. astro-ph/0003477

    Pith/arXiv arXiv 2000

  68. [68]

    2022, title Signatures of spin precession and nutation in isolated black-hole binaries , Phys

    Steinle, N., & Kesden, M. 2022, title Signatures of spin precession and nutation in isolated black-hole binaries , Phys. Rev. D, 106, 063028, 10.1103/PhysRevD.106.063028

    doi:10.1103/physrevd.106.063028 2022

  69. [69]

    Mandel , Riley , J., Boesky , A., et al

    Team COMPAS: I. Mandel , Riley , J., Boesky , A., et al. 2025, title Rapid Stellar and Binary Population Synthesis with COMPAS: Methods Paper II , Astrophys. J. Supp. S., 280, 43, 10.3847/1538-4365/adf8d0

    doi:10.3847/1538-4365/adf8d0 2025

  70. [70]

    Riley , et al

    Team COMPAS: J. Riley , et al. 2022, title Rapid Stellar and Binary Population Synthesis with COMPAS , Astrophys. J. Supp., 258, 34, 10.3847/1538-4365/ac416c

    doi:10.3847/1538-4365/ac416c 2022

  71. [71]

    Terquem, C., Papaloizou, J. C. B., Nelson, R. P., & Lin, D. N. C. 1998, title On the tidal interaction of a solar-type star with an orbiting companion: excitation of g mode oscillation and orbital evolution , Astrophys. J., 502, 788, 10.1086/305927

    doi:10.1086/305927 1998

  72. [72]

    Tokovinin, A., & Latham, D. W. 2020, title Orbits of Five Triple Stars, The Astronomical Journal, 160, 251

    2020

  73. [73]

    G., Prusti, T., et al

    Vallenari, A., Brown, A. G., Prusti, T., et al. 2023, title Gaia data release 3-summary of the content and survey properties, Astronomy & Astrophysics, 674, A1

    2023

  74. [74]

    1995, title Tidal circularization and the eccentricity of binaries containing giant stars., Astronomy and Astrophysics, v

    Verbunt, F., & Phinney, E. 1995, title Tidal circularization and the eccentricity of binaries containing giant stars., Astronomy and Astrophysics, v. 296, p. 709, 296, 709

    1995

  75. [75]

    Vidal, J., & Barker, A. J. 2020, title Efficiency of tidal dissipation in slowly rotating fully convective stars or planets, Monthly Notices of the Royal Astronomical Society, 497, 4472

    2020

  76. [76]

    1966, title Les mar \'e es dans une \'e toile double serr \'e e, Annales d'Astrophysique, Vol

    Zahn, J.-P. 1966, title Les mar \'e es dans une \'e toile double serr \'e e, Annales d'Astrophysique, Vol. 29, p. 313, 29, 313

    1966

  77. [77]

    Zahn , J. P. 1975, title The dynamical tide in close binaries. , Astronomy and Astrophysics, 41, 329

    1975

  78. [78]

    1977, title Tidal friction in close binary systems., Astronomy and Astrophysics, 57, 383

    Zahn, J.-P. 1977, title Tidal friction in close binary systems., Astronomy and Astrophysics, 57, 383

    1977

  79. [79]

    1989, title Tidal evolution of close binary stars

    Zahn, J.-P., & Bouchet, L. 1989, title Tidal evolution of close binary stars. II-Orbital circularization of late-type binaries, Astronomy and Astrophysics (ISSN 0004-6361), vol. 223, no. 1-2, Oct. 1989, p. 112-118., 223, 112

    1989