REVIEW 3 major objections 5 minor 271 references
On the Eccentricity Distribution and Tidal Evolution of Transiting Brown Dwarfs
T0 review · 3 major / 5 minor · reviewed 2026-07-12 · grok-4.5
Pith's one-line read Transiting brown dwarfs share one primordial eccentricity distribution that tides later circularise, yielding a typical tidal quality factor of order 10^7–10^8.
desk verdict Solid first population Q_BD from the eccentricity split of the full known transiting-BD sample; the number is useful but rests on an N=8 primordial Beta and equilibrium tides. read the letter →
The pith
A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.
The reading
What carries the argument
A hierarchical Bayesian Beta model for the eccentricity distribution, split at the Kolmogorov–Smirnov-selected period threshold of 16 days, combined with orbit-averaged tidal evolution equations (Wisdom 2008 and Jackson et al. 2008) that are sampled until the evolved distribution minimises the Kullback–Leibler divergence to the observed short-period sample.
What would settle it
A statistically larger sample of long-period (P ≳ 16 d) transiting brown dwarfs whose eccentricity distribution is inconsistent with the Beta(1.88, 2.47) parent that was used to seed the short-period population would falsify the shared-primordial-distribution premise and therefore the derived Q values.
Extended reading notes
Core claim
Assuming the full set of transiting brown dwarfs began with the same primordial eccentricity distribution that is still observed among the longer-period systems (a Beta distribution with shape parameters α ≈ 1.88, β ≈ 2.47), the short-period population is the tidally circularised remnant of that distribution. Forward modelling under two equilibrium-tide prescriptions then yields a typical brown-dwarf tidal quality factor Q_BD = 10^{8.1±1.0} when only brown-dwarf tides are considered, or Q_BD = 10^{7.1±0.3} together with a stellar quality factor Q_⋆ = 10^{6.0±0.1} when tides raised on the host star are included.
Load-bearing premise
That every short-period brown dwarf started with the same eccentricity distribution that we still see among the longer-period ones, so the difference between the two samples is produced only by later tidal damping.
Editorial extensions
If this is right
- Brown dwarfs dissipate tidal energy far less efficiently than hot Jupiters, so even short-period systems can preserve orbital signatures of formation.
- Population-level eccentricity statistics become a practical route to measuring effective tidal quality factors for objects whose individual ages and interior structures are poorly known.
- The longer-period transiting brown-dwarf sample is kinematically closer to close stellar binaries than to giant planets, favouring a star-like formation channel for the bulk of the present sample.
- Future transit surveys that enlarge the long-period brown-dwarf census will directly tighten or refute the Q constraints without requiring new tidal theory.
Reading between the lines
- If lower-mass brown dwarfs (near the deuterium-burning limit) form by a different channel, they may possess systematically different Q values that are invisible in the current high-mass-dominated sample.
- The same hierarchical-plus-tidal-evolution pipeline could be applied to the growing sample of transiting very-low-mass stars to test whether the derived Q continuum is continuous across the hydrogen-burning limit.
- Because the inferred Q is an effective, frequency-averaged quantity, multi-frequency or resonance-locking models of brown-dwarf interiors may still be consistent with the same population-level numbers.
Signed reviews
Editorial analysis
A structured set of objections, weighed in public.
Referee Report
Summary. The paper uniformly re-fits archival RVs for 50 transiting BD/low-mass-star systems (retaining 36 with M_b sin i < 75 M_Jup) and uses a hierarchical Bayesian Beta model to characterise the eccentricity distribution. A KS-selected period cut at 16 days separates a short-period population (N=28) that is skewed toward low e (Beta with α<1, β>1) from a long-period population (N=8) that is more dynamically excited (α,β>1). Under the assumption that both populations share a single primordial eccentricity distribution equal to the observed LP Beta, the authors forward-model tidal evolution with the Wisdom (2008) and Jackson et al. (2008) equilibrium-tide formalisms and minimise KL divergence to the observed SP distribution, obtaining Q_BD = 10^{8.1±1.0} (Model A) or Q_BD = 10^{7.1±0.3} and Q_⋆ = 10^{6.0±0.1} (Model B). They conclude that BDs dissipate tidal energy less efficiently than hot Jupiters and more like low-mass stars, so that even short-period BDs can retain formation-era orbital imprints.
Significance. If the single-primordial-distribution assumption holds, the work supplies one of the first population-level empirical constraints on the effective tidal quality factor of brown dwarfs, placing them intermediate between gas giants and low-mass stars. The uniform RV re-analysis, hierarchical Beta modelling, and transparent forward-modelling pipeline (bootstrap of SP masses/periods, angular-momentum conservation, KL minimisation) are cleanly executed and make the result reproducible. The comparison to CLS giant planets, Gaia binaries, and recent low-mass-star samples usefully situates the BD population. The result is therefore of genuine interest for both tidal theory and formation pathways of the planet–BD continuum, even though the numerical Q values rest on a small LP sample.
major comments (3)
- The central Q inference (§4.3 and abstract) treats the LP Beta B(1.879,2.470) as the universal primordial eccentricity distribution for every SP system. That Beta is fit to only N=8 objects (Table 1, Fig. 2). Because every initial eccentricity in the forward model is drawn from this fixed distribution, sampling variance or selection bias in the LP fit propagates directly into the reported Q_BD (and Q_⋆). The paper notes the small LP sample in §5 but still quotes a single point estimate. At minimum the authors should (i) re-draw the LP hyperparameters from their full posterior at each realisation, (ii) report the resulting systematic uncertainty on log Q, and (iii) test an alternative prior (e.g., the full-sample Beta or a thermal distribution) so that the reader can judge how load-bearing the N=8 fit is.
- The evolutionary age is fixed at the median 6.5 Gyr for the primary result (§4.3). The authors later show that Q_BD rises monotonically from ~10^{7.6} at 1 Gyr to ~10^{8.3} at 13 Gyr (Model A). Because the true age distribution is broad, a single-age KL minimum understates the uncertainty. Propagating the observed age distribution (or at least a realistic prior) through the same MCMC would give a more honest posterior on Q.
- Both tidal models are pure equilibrium-tide prescriptions that omit dynamical tides, inertial-wave dissipation, and resonance locking (explicitly acknowledged in §4). The inferred Q is therefore an effective, frequency-averaged parameter. The abstract and conclusions should state this limitation more prominently so that the numerical values are not over-interpreted as fundamental material constants of BDs.
minor comments (5)
- The period threshold is chosen by minimising the one-sided KS p-value over a 1–40 day grid (§3.2). A brief statement of how sensitive the subsequent Beta parameters and Q values are to neighbouring thresholds (e.g., 12 or 20 days) would strengthen the claim that 16 days is robust.
- Figure 1 caption and the angular-momentum tracks use e = sqrt(1-(P0/P)^{2/3}); the same relation appears later as P_final = P_initial (1-e0^{2})^{3/2}. A single consistent notation would avoid confusion.
- Table 1 reports mean eccentricities with asymmetric Beta-parameter uncertainties; adding the corresponding 16th/84th percentiles of the mean-e posterior would make the table self-contained.
- The Love number κ2 appears in Eq. (5) but is never assigned a numerical value or prior; a short statement of the adopted value (or that it is absorbed into the effective Q) is needed.
- A few typographical inconsistencies remain (e.g., “T ransiting” in the title line, mixed Q vs. Q' notation early in the introduction). A careful proof-read would clean these up.
Circularity Check
No significant circularity: Q is ordinary KL-minimizing fit of external tidal models under an explicit shared-primordial assumption; SP/LP Betas are independent data products.
full rationale
The paper first re-fits RVs uniformly (§2), then independently fits Beta hyperparameters to the SP (N=28) and LP (N=8) eccentricity samples via HBM (§3.2, Table 1). The period split itself is data-driven (KS test). In §4.3 it explicitly assumes the LP Beta B(1.879,2.470) is the common primordial distribution, draws initial e from it, evolves the SP periods/masses under the external Wisdom (2008) or Jackson et al. (2008) equations while varying log Q on a grid, and reports the Q that minimises KL divergence to the independently observed SP Beta. The tidal ODEs and the two eccentricity data products are independent; nothing forces a good match for any particular Q (they simply find one). The assumption is strong and the LP sample small (noted in §5), but that is a modelling/data limitation, not a reduction of the claimed Q to its inputs by construction. No self-citation is load-bearing for uniqueness or the tidal formalisms; no ansatz is smuggled; no fitted quantity is renamed a prediction. Score 1 only for the mild presentation of a conditional fit as a population constraint.
Assumptions & free parameters
free parameters (4)
- Beta hyperparameters (α,β) for SP, LP, and full samples =
SP: (0.426^{+0.100}_{-0.084}, 2.354^{+0.807}_{-0.658}); LP: (1.879^{+1.088}_{-0.753}, 2.470^{+1.480}_{-1.018})
- Period threshold P_threshold =
16 days
- Evolutionary age =
6.5 Gyr
- Q_BD (and Q_⋆ in Model B) =
Model A: 10^{8.1±1.0}; Model B: Q_BD=10^{7.1±0.3}, Q_⋆=10^{6.0±0.1}
assumptions (6)
- domain assumption Orbital eccentricities of bound companions are well described by a Beta distribution on [0,1].
- domain assumption Wisdom (2008) equilibrium-tide equations (only BD tide, synchronous rotation, low-e expansion) correctly capture the secular ė of the population.
- domain assumption Jackson et al. (2008) coupled star+planet equilibrium-tide equations correctly capture ė and ȧ.
- domain assumption Angular momentum is conserved during circularization, so P_final = P_initial (1-e0²)^{3/2}.
- ad hoc to paper Short-period and long-period transiting BDs share a single primordial eccentricity distribution identical to the observed long-period Beta.
- domain assumption Dynamical tides, inertial-wave dissipation, resonance locking and structural feedback from tidal heating can be neglected or absorbed into an effective constant Q.
Cite this review
Pith. "Pith review of On the Eccentricity Distribution and Tidal Evolution of Transiting Brown Dwarfs." pith.science (2026). https://pith.science/paper/JLM5O42S
@misc{pith2026260702682,
author = {Pith},
title = {Pith review of: On the Eccentricity Distribution and Tidal Evolution of Transiting Brown Dwarfs},
year = {2026},
howpublished = {\url{https://pith.science/paper/JLM5O42S}},
note = {Machine review of arXiv:2607.02682}
}
abstract
Brown dwarfs on short-period orbits populate an intermediate regime between hot Jupiters and tight stellar binaries, lying at the intersection of possible evolutionary avenues. Their orbital eccentricities retain the dynamical imprint of both their formation pathways and any subsequent tidal evolution, providing a diagnostic for whether such objects formed in situ at small separations or were driven inward from higher-eccentricity orbits shaped by tidal dissipation. Using a hierarchical Bayesian framework, we characterise the orbital eccentricity distribution of transiting brown dwarfs. Short-period brown dwarfs ($P < 16$ days) are well represented by a Beta distribution with $\alpha < 1$ and $\beta > 1$, indicating a population concentrated at low eccentricities, whereas longer-period brown dwarfs ($P \geq 16$ days) display $\alpha,~\beta > 1$ and therefore occupy a more dynamically excited regime. This difference in eccentricity distributions likely reflects corresponding differences in the populations' eccentricity-damping timescales: close-in systems may evolve toward circular orbits on relatively short timescales, whilst wider companions experience negligible tidal processing over their lifetimes. Assuming that the full set of transiting brown dwarfs stems from a single primordial eccentricity distribution, {we constrain the typical brown dwarf tidal quality factor to $\mathcal{Q}_{\rm BD} = 10^{8.1\pm1.0}$ when neglecting the influence of tides raised on the host star, or $\mathcal{Q}_{\rm BD} = 10^{7.1\pm0.3}$ and $\mathcal{Q}_{\star} = 10^{6.0\pm0.1}$ when they are included.
Figures
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Reference graph
Works this paper leans on
-
[1]
, year = 1963, month = may, volume =
The Structure of Stars of Very Low Mass. , year = 1963, month = may, volume =. doi:10.1086/147589 , adsurl =
doi:10.1086/147589 1963
-
[2]
, year = 1919, month = apr, volume =
The origin of binary systems. , year = 1919, month = apr, volume =. doi:10.1093/mnras/79.6.408 , adsurl =
-
[3]
, year = 1963, month = may, volume =
The Helmholtz-Kelvin Time Scale for Stars of Very Low Mass. , year = 1963, month = may, volume =. doi:10.1086/147590 , adsurl =
-
[4]
A Nongray Theory of Extrasolar Giant Planets and Brown Dwarfs. , keywords =. doi:10.1086/305002 , archivePrefix =. astro-ph/9705201 , primaryClass =
-
[5]
Origins of Hot Jupiters. , keywords =. doi:10.1146/annurev-astro-081817-051853 , archivePrefix =. 1801.06117 , primaryClass =
-
[6]
Population-level Eccentricity Distributions of Imaged Exoplanets and Brown Dwarf Companions: Dynamical Evidence for Distinct Formation Channels. , keywords =. doi:10.3847/1538-3881/ab5b11 , archivePrefix =. 1911.10569 , primaryClass =
work page Pith review arXiv doi:10.3847/1538-3881/ab5b11 1911
-
[7]
Statistical Properties of Brown Dwarf Companions: Implications for Different Formation Mechanisms
Statistical properties of brown dwarf companions: implications for different formation mechanisms. , keywords =. doi:10.1093/mnras/stu134 , archivePrefix =. 1303.6442 , primaryClass =
-
[8]
, year = 1996, month = nov, volume =
Formation of the Giant Planets by Concurrent Accretion of Solids and Gas. , year = 1996, month = nov, volume =. doi:10.1006/icar.1996.0190 , adsurl =
Show all 271 references
- [9]
- [10]
- [11]
- [12]
- [13]
- [14]
- [15]
- [16]
- [17]
- [18]
-
[19]
arXiv e-prints , keywords =
Evidence for a Peak at 0.3 in the Eccentricity Distribution of Typical Super-Jovian Exoplanets. arXiv e-prints , keywords =. doi:10.48550/arXiv.2601.18877 , archivePrefix =. 2601.18877 , primaryClass =
- [20]
- [21]
- [22]
- [23]
- [24]
- [25]
- [26]
-
[27]
Monographs on Environment, Earth and Planets , keywords =
The Lidov-Kozai Oscillation and Hugo von Zeipel. Monographs on Environment, Earth and Planets , keywords =. doi:10.5047/meep.2019.00701.0001 , archivePrefix =. 1911.03984 , primaryClass =
2019 doi
- [28]
- [29]
- [30]
- [31]
- [32]
- [33]
- [34]
- [35]
-
[36]
, year = 1962, month = nov, volume =
Secular perturbations of asteroids with high inclination and eccentricity. , year = 1962, month = nov, volume =. doi:10.1086/108790 , adsurl =
1962 doi
-
[37]
, year = 1962, month = oct, volume =
The evolution of orbits of artificial satellites of planets under the action of gravitational perturbations of external bodies. , year = 1962, month = oct, volume =. doi:10.1016/0032-0633(62)90129-0 , adsurl =
1962 doi
- [38]
-
[39]
Dynamics of Planetary Systems
- [40]
- [41]
- [42]
- [43]
-
[44]
, keywords =
The Origin of Binary Stars. , keywords =. doi:10.1146/annurev.astro.40.060401.093810 , adsurl =
- [45]
- [46]
- [47]
-
[48]
PyMC3: Python probabilistic programming framework
-
[49]
Statistical Science , year = 1992, month = jan, volume =
Inference from Iterative Simulation Using Multiple Sequences. Statistical Science , year = 1992, month = jan, volume =. doi:10.1214/ss/1177011136 , adsurl =
1992 doi
- [50]
- [51]
- [52]
- [53]
- [54]
- [55]
- [56]
-
[57]
Science , keywords =
Dynamical instabilities and the formation of extrasolar planetary systems. Science , keywords =. doi:10.1126/science.274.5289.954 , adsurl =
- [58]
-
[59]
, year = 1937, month = jan, volume =
On the Statistics of Double Stars. , year = 1937, month = jan, volume =
1937
-
[60]
Bayesian Data Analysis
- [61]
-
[62]
Annual Review of Earth and Planetary Sciences , keywords =
Planetesimals to Brown Dwarfs: What is a Planet?. Annual Review of Earth and Planetary Sciences , keywords =. doi:10.1146/annurev.earth.34.031405.125058 , archivePrefix =. astro-ph/0608417 , primaryClass =
-
[63]
doi:10.1007/3-540-27610-6 , adsurl =
New light on dark stars : red dwarfs, low-mass stars, brown dwarfs. doi:10.1007/3-540-27610-6 , adsurl =
- [64]
- [65]
- [66]
- [67]
-
[68]
Table of integrals, series and products
-
[69]
and Anderson, D.R
Burnham, K.P. and Anderson, D.R. , biburl =. Model selection and multimodel inference: a practical information-theoretic approach , username =
-
[70]
, year = 1966, month = jan, volume =
Q in the Solar System. , year = 1966, month = jan, volume =. doi:10.1016/0019-1035(66)90051-0 , adsurl =
1966 doi
-
[71]
, keywords =
The formation of planetary systems. , keywords =. doi:10.1111/j.1365-2966.2004.07417.x , adsurl =
2004 doi
-
[72]
, keywords =
Tidal decay and orbital circularization in close-in two-planet systems. , keywords =. doi:10.1111/j.1365-2966.2011.18861.x , archivePrefix =. 1104.0964 , primaryClass =
2011 doi
- [73]
-
[74]
, year = 2007, month = jun, volume =
A new catalogue of eclipsing binary stars with eccentric orbits*. , year = 2007, month = jun, volume =. doi:10.1111/j.1365-2966.2007.11756.x , adsurl =
2007 doi
- [75]
- [76]
- [77]
- [78]
- [79]
-
[80]
American Astronomical Society Meeting Abstracts , year = 2022, series =
The Impact of Bayesian Hyperpriors on the Population-Level Eccentricity Distribution of Imaged Planets. American Astronomical Society Meeting Abstracts , year = 2022, series =
2022
-
[81]
, keywords =
Criteria for fragmentation in a collapsing rotating cloud. , keywords =. doi:10.1086/158457 , adsurl =
-
[82]
, keywords =
Collapse of a molecular cloud core to stellar densities: the formation and evolution of pre-stellar discs. , keywords =. doi:10.1111/j.1365-2966.2011.19386.x , archivePrefix =. 1108.0009 , primaryClass =
2011 doi
- [83]
-
[84]
, year = 1976, month = sep, volume =
Opacity-limited hierarchical fragmentation and the masses of protostars. , year = 1976, month = sep, volume =. doi:10.1093/mnras/176.3.483 , adsurl =
1976 doi
-
[85]
doi:10.1007/978-3-642-30304-3 , adsurl =
Stellar Structure and Evolution. doi:10.1007/978-3-642-30304-3 , adsurl =
-
[86]
European Physical Journal Web of Conferences , year = 2013, series =
The formation of planets by disc fragmentation. European Physical Journal Web of Conferences , year = 2013, series =. doi:10.1051/epjconf/20134708001 , archivePrefix =. 1302.3955 , primaryClass =
2013 doi
-
[87]
Mathematical methods for physicists 6th ed
- [88]
-
[89]
Bulletin Moscow University , volume=
Estimate of deviation between empirical distribution functions in two independent samples , author=. Bulletin Moscow University , volume=
-
[90]
Giorn Dell'inst Ital Degli Att , volume=
Sulla determinazione empirica di una legge didistribuzione , author=. Giorn Dell'inst Ital Degli Att , volume=
- [91]
-
[92]
Savonije, G. J. and Papaloizou, J. C. B. Tidal Interactions of Close Binary Systems. Interacting Binaries. 1985. doi:10.1007/978-94-009-5337-6_4
1985 doi
- [93]
- [94]
-
[95]
Tidal Evolution and Oscillations in Binary Stars , year = 2005, editor =
Physical mechanisms for tidal dissipation. Tidal Evolution and Oscillations in Binary Stars , year = 2005, editor =
2005
- [96]
- [97]
-
[98]
9th Python in Science Conference , year=
statsmodels: Econometric and statistical modeling with python , author=. 9th Python in Science Conference , year=
- [99]
- [100]
- [101]
- [102]
-
[103]
doi:10.5281/zenodo.3509134 , version =
pandas-dev/pandas: Pandas. doi:10.5281/zenodo.3509134 , version =
-
[104]
Computing in Science and Engineering , keywords =
Matplotlib: A 2D Graphics Environment. Computing in Science and Engineering , keywords =. doi:10.1109/MCSE.2007.55 , adsurl =
2007 doi
- [105]
-
[106]
, year = 1969, month = jan, volume =
Numerical calculations of the dynamics of collapsing proto-star. , year = 1969, month = jan, volume =. doi:10.1093/mnras/145.3.271 , adsurl =
1969 doi
-
[107]
, keywords =
Orbital eccentricity growth through disc-companion tidal interaction. , keywords =. doi:10.1051/0004-6361:20000011 , adsurl =
- [108]
- [109]
- [110]
-
[111]
Communications in Applied Mathematics and Computational Science , keywords =
Ensemble samplers with affine invariance. Communications in Applied Mathematics and Computational Science , keywords =. doi:10.2140/camcos.2010.5.65 , adsurl =
2010 doi
- [112]
-
[113]
, year = 1971, month = aug, volume =
Spectroscopic binaries with circular orbits. , year = 1971, month = aug, volume =. doi:10.1086/111159 , adsurl =
1971 doi
-
[114]
The anomalous temperature reversal in the context of tidal heating
Tidal effects on brown dwarfs: application to the eclipsing binary 2MASS J05352184-0546085. The anomalous temperature reversal in the context of tidal heating. , keywords =. doi:10.1051/0004-6361/200912826 , archivePrefix =. 1002.1246 , primaryClass =
- [115]
- [116]
- [117]
- [118]
- [119]
-
[120]
Science , keywords =
Giant planet formation by gravitational instability. Science , keywords =. doi:10.1126/science.276.5320.1836 , adsurl =
-
[121]
, keywords =
The formation mechanism of brown dwarfs. , keywords =. doi:10.1046/j.1365-8711.2002.05539.x , archivePrefix =. astro-ph/0206365 , primaryClass =
2002 doi
- [122]
- [123]
- [124]
- [125]
- [126]
- [127]
- [128]
- [129]
- [130]
- [131]
-
[132]
I - Revisiting the theory of the equilibrium tide
Tidal evolution of close binary stars. I - Revisiting the theory of the equilibrium tide. , keywords =
- [133]
-
[134]
, keywords =
Tidal evolution in close binary systems. , keywords =
-
[135]
, year = 2008, month = feb, volume =
Tidal dissipation at arbitrary eccentricity and obliquity. , year = 2008, month = feb, volume =. doi:10.1016/j.icarus.2007.09.002 , adsurl =
2008 doi
- [136]
- [137]
- [138]
- [139]
-
[140]
Proceedings of the Fifth Berkeley Symposium on Mathematical Statistics and Probability, Volume 1: Statistics , volume=
Some methods for classification and analysis of multivariate observations , author=. Proceedings of the Fifth Berkeley Symposium on Mathematical Statistics and Probability, Volume 1: Statistics , volume=. 1967 , organization=
1967
-
[141]
Main source (Gaia Collaboration, 2022)
VizieR Online Data Catalog: Gaia DR3 Part 1. Main source (Gaia Collaboration, 2022). doi:10.26093/cds/vizier.1355 , adsurl =
2022 doi
- [142]
- [143]
-
[144]
, keywords =
Gravitational fragmentation and the formation of brown dwarfs in stellar clusters. , keywords =. doi:10.1111/j.1365-2966.2008.13679.x , archivePrefix =. 0807.0460 , primaryClass =
2008 doi
- [145]
- [146]
-
[147]
, keywords =
The properties of brown dwarfs and low-mass hydrogen-burning stars formed by disc fragmentation. , keywords =. doi:10.1111/j.1365-2966.2008.14069.x , archivePrefix =. 0810.1687 , primaryClass =
2008 doi
- [148]
- [149]
- [150]
- [151]
-
[152]
doi:10.5281/zenodo.14249941 , version =
Matplotlib: Visualization with Python. doi:10.5281/zenodo.14249941 , version =
- [153]
-
[154]
The Journal of Open Source Software , year = 2016, month = jun, volume =
corner.py: Scatterplot matrices in Python. The Journal of Open Source Software , year = 2016, month = jun, volume =. doi:10.21105/joss.00024 , adsurl =
2016 doi
-
[155]
doi:10.5281/zenodo.593847 , version =
statsmodels/statsmodels: Release 0.14.2. doi:10.5281/zenodo.593847 , version =
-
[156]
The Journal of Open Source Software , keywords =
ArviZ a unified library for exploratory analysis of Bayesian models in Python. The Journal of Open Source Software , keywords =. doi:10.21105/joss.01143 , adsurl =
-
[157]
doi:10.5281/zenodo.3767070 , version =
mwaskom/seaborn: v0.10.1 (April 2020). doi:10.5281/zenodo.3767070 , version =
2020 doi
- [158]
- [159]
- [160]
- [161]
- [162]
- [163]
- [164]
- [165]
- [166]
- [167]
- [168]
- [169]
- [170]
- [171]
- [172]
- [173]
- [174]
- [175]
- [176]
- [177]
- [178]
-
[179]
OGLE-TR-123
Radius and mass of a transiting M dwarf near the hydrogen-burning limit. OGLE-TR-123. , keywords =. doi:10.1051/0004-6361:20053692 , adsurl =
- [180]
-
[181]
, keywords =
TOI-503: The First Known Brown-dwarf Am-star Binary from the TESS Mission. , keywords =. doi:10.3847/1538-3881/ab7245 , archivePrefix =. 1909.07984 , primaryClass =
1909 doi
- [182]
- [183]
- [184]
- [185]
- [186]
- [187]
- [188]
- [189]
- [190]
- [191]
- [192]
- [193]
- [194]
- [195]
- [196]
- [197]
- [198]
-
[199]
, keywords =
Frequency Dependence of Tidal q. , keywords =. doi:10.1088/0004-637X/698/1/L42 , adsurl =
-
[200]
The CoRoT Legacy Book: The Adventure of the Ultra High Precision Photometry from Space , year = 2016, pages =
III.9-2 Tidal evolution of CoRoT massive planets and brown dwarfs and of their host stars. The CoRoT Legacy Book: The Adventure of the Ultra High Precision Photometry from Space , year = 2016, pages =. doi:10.1051/978-2-7598-1876-1.c239 , adsurl =
2016 doi
- [201]
-
[202]
Studies of Stellar Rotation. V. The Dependence of Rotation on Age among Solar-Type Stars. , year = 1967, month = nov, volume =. doi:10.1086/149359 , adsurl =
1967 doi
- [203]
- [204]
- [205]
- [206]
-
[207]
Lindstedt \`a l' \'e tude du mouvement des com \`e tes p \'e riodiques
Sur l'application des s \'e ries de M. Lindstedt \`a l' \'e tude du mouvement des com \`e tes p \'e riodiques. Astronomische Nachrichten , year = 1910, month = mar, volume =. doi:10.1002/asna.19091832202 , adsurl =
1910 doi
-
[208]
and Leibler, R
Kullback, S. and Leibler, R. A. On Information and Sufficiency. The Annals of Mathematical Statistics. 1951. doi:10.1214/aoms/1177729694
1951 doi
- [209]
- [210]
- [211]
- [212]
- [213]
-
[214]
, keywords =
Turbulent Fragmentation and Star Formation. , keywords =. doi:10.1023/B:ASTR.0000045018.50154.b0 , archivePrefix =. astro-ph/0311319 , primaryClass =
- [215]
- [216]
- [217]
- [218]
- [219]
- [220]
- [221]
- [222]
- [223]
- [224]
- [225]
-
[226]
, keywords =
How tidal heating in Io drives the galilean orbital resonance locks. , keywords =. doi:10.1038/279767a0 , adsurl =
-
[227]
Lunar and Planetary Science Conference , year = 1980, series =
On the Q of Jupiter. Lunar and Planetary Science Conference , year = 1980, series =
1980
-
[228]
AAS/Division for Planetary Sciences Meeting Abstracts \#40 , year = 2008, series =
Jupiter's Tidal Q: The Range of Uncertainty. AAS/Division for Planetary Sciences Meeting Abstracts \#40 , year = 2008, series =
2008
-
[229]
, keywords =
Turbulent Viscosity and Jupiter's Tidal Q. , keywords =. doi:10.1016/0019-1035(77)90163-4 , adsurl =
- [230]
- [231]
- [232]
-
[233]
, keywords =
Tidal friction in close binary systems. , keywords =
- [234]
- [235]
- [236]
- [237]
- [238]
- [239]
- [240]
- [241]
- [242]
-
[243]
, keywords =
Distinct Rotational Evolution of Giant Planets and Brown Dwarf Companions. , keywords =. doi:10.3847/1538-3881/ae434b , archivePrefix =. 2601.05976 , primaryClass =
- [244]
-
[245]
, keywords =
Structural Effects of Magnetic Fields in Brown Dwarfs. , keywords =. doi:10.1088/0004-637X/700/1/387 , adsurl =
- [246]
-
[247]
, keywords =
Magnetic Models of the Brown Dwarfs HD 130948b and HD 130948c. , keywords =. doi:10.1088/0004-637X/713/2/1249 , adsurl =
- [248]
-
[249]
Weather on Other Worlds. V. The Three Most Rapidly Rotating Ultra-cool Dwarfs. , keywords =. doi:10.3847/1538-3881/abeb67 , archivePrefix =. 2103.01990 , primaryClass =
- [250]
- [251]
- [252]
- [253]
-
[254]
, keywords =
Orbital Eccentricities Suggest a Gradual Transition from Giant Planets to Brown Dwarfs. , keywords =. doi:10.3847/1538-3881/ae1fd7 , archivePrefix =. 2511.12816 , primaryClass =
-
[255]
Philosophical Transactions of the Royal Society of London Series I , year = 1879, month = jan, volume =
On the Precession of a Viscous Spheroid, and on the Remote History of the Earth. Philosophical Transactions of the Royal Society of London Series I , year = 1879, month = jan, volume =
-
[256]
Philosophical Transactions of the Royal Society of London Series I , year = 1880, month = jan, volume =
On the Secular Changes in the Elements of the Orbit of a Satellite Revolving about a Tidally Distorted Planet. Philosophical Transactions of the Royal Society of London Series I , year = 1880, month = jan, volume =
-
[257]
Reviews of Geophysics and Space Physics , year = 1964, month = jan, volume =
Tidal Dissipation by Solid Friction and the Resulting Orbital Evolution. Reviews of Geophysics and Space Physics , year = 1964, month = jan, volume =. doi:10.1029/RG002i004p00661 , adsurl =
1964 doi
-
[258]
Reviews of Geophysics and Space Physics , year = 1964, month = jan, volume =
Tidal Friction. Reviews of Geophysics and Space Physics , year = 1964, month = jan, volume =. doi:10.1029/RG002i003p00467 , adsurl =
1964 doi
-
[259]
Annales d'Astrophysique , year = 1966, month = feb, volume =
Les mar \'e es dans une \'e toile double serr \'e e (suite). Annales d'Astrophysique , year = 1966, month = feb, volume =
1966
-
[260]
, keywords =
Tidal Evolution in Close Binary Systems. , keywords =. doi:10.1007/BF00642550 , adsurl =
-
[261]
, keywords =
The dynamical tide in close binaries. , keywords =
- [262]
- [263]
-
[264]
Moon and Planets , keywords =
The Evolution of the Lunar Orbit Revisited - Part Two. Moon and Planets , keywords =. doi:10.1007/BF00899817 , adsurl =
-
[265]
Best, William M. J. and Dupuy, Trent J. and Liu, Michael C. and Sanghi, Aniket and Siverd, Robert J. and Zhang, Zhoujian , title =. doi:10.5281/zenodo.15802304 , url =
- [266]
-
[267]
New determination of the hydrogen burning limit
Impact of a new H/He equation of state on the evolution of massive brown dwarfs. New determination of the hydrogen burning limit. , keywords =. doi:10.1051/0004-6361/202243832 , archivePrefix =. 2212.07153 , primaryClass =
- [268]
- [269]
-
[270]
Astrobiology , keywords =
Tidal Heating of Earth-like Exoplanets around M Stars: Thermal, Magnetic, and Orbital Evolutions. Astrobiology , keywords =. doi:10.1089/ast.2015.1325 , archivePrefix =. 1509.07452 , primaryClass =
2015 doi
- [271]
Reviewed July 12, 2026 · model on record in the stance chip above.
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