Formation of Compact Hierarchical Triples

Ayush Moharana; G. Pawar; K.G. Helminiak; T. Pawar

REVIEW 3 major objections 5 minor 1 cited by

Formation of Compact Hierarchical Triples

T0 review · 3 major / 5 minor · reviewed 2026-08-12 · deepseek-v4-flash

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗ Review JSON

Pith's one-line read The observed mass-ratio and eccentricity distributions of compact hierarchical triples favor sequential disk-instability formation, with a bimodal mass-ratio split between old and young systems.

desk verdict A useful, honest conference paper that combines the three main CHT catalogs for the first time, but the central age/metallicity interpretation rests on an unexamined fixed-mass assumption and should be treated as a suggestion, not a result. read the letter →

arxiv 2411.11459 v1 pith:Z6HSRXZE submitted 2024-11-18 astro-ph.SR

Ayush Moharana , K.G. Helminiak , T. Pawar , G. Pawar This is my paper · ORCID

classification astro-ph.SR

keywords compacthierarchicaltriplestriplestarformationdiskinstabilityeclipsetimingvariationsGaianon-singlestarsmassratiodistributioneccentricityGalacticbulge

verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

Compact hierarchical triples are three-star systems whose outermost orbit is shorter than 1000 days. This paper combines eclipse-timing samples from Kepler and OGLE with Gaia astrometric orbits to reconstruct, for the first time across surveys, the outer mass-ratio and eccentricity distributions of these systems. It finds that the mass-ratio distribution is bimodal, with a low-q3 peak dominated by old Galactic Bulge systems from OGLE and a high-q3 peak from younger Gaia and Kepler systems. The eccentricity distribution sits above a flat distribution and differs between surveys in a way the authors tie to metallicity. The authors argue both distributions are consistent with sequential disk-instability formation plus later dynamical mass loss, and they identify the specific dynamical mechanisms (tidal dissipation, circumbinary disk interactions) that could drive the mass-ratio shift.

What carries the argument

The key machinery is the transformation of each survey's orbital parameters into a common tertiary mass ratio q3 = mC/mbin using Kepler's mass function f(m3) = P2 $K^{3}$ / (2 pi G) (1 - $e2^{2}$)^{3/2}, converted into the cubic equation mbin $q3^{3}$ - f $q3^{2}$ - 2f q3 - f = 0 (Eq. 2). For ETV surveys f is measured directly; for Gaia, the paper approximates K = 2 pi a2 / P2 and sets e2 = 0, and for all surveys it assumes mbin = 2 solar masses. This common q3 scale is what allows the distributions to be compared across surveys, and its approximations carry the argument.

What would settle it

Recompute the q3 distribution using measured inner binary masses (from double-lined eclipsing binaries) and actual Gaia eccentricities for a subsample of CHTs: if the bimodality disappears or the low-q3 peak shifts, the two-population age interpretation is wrong. Alternatively, direct age measurements of the OGLE Bulge CHTs that show they are not old would falsify the age assignment.

Watch

Extended reading notes

Core claim

The central claim is that the observed eccentricity and tertiary mass-ratio distributions of compact hierarchical triples are consistent with a single formation channel: sequential disk instability (DI+DI). The mass-ratio distribution is bimodal, with peaks at q3 about 0.2-0.35 and near q3 = 1; the low-q3 peak is populated almost entirely by the OGLE Bulge sample, which the authors interpret as old CHTs, while the high-q3 peak comes from younger GAIA/Kepler systems. The eccentricity distribution is right-shifted relative to flat, and the survey-by-survey differences at low eccentricity are interpreted as a metallicity signal. Taken together, the paper concludes that CHTs form through disk fragmentation in the circumbinary disk and then evolve through mass loss from tidal dissipation or interactions with the circumbinary accretion disk, which moves systems from high to low q3 over gigayears.

Load-bearing premise

The whole mass-ratio distribution assumes every inner binary has a total mass of 2 solar masses and that Gaia outer orbits can be treated as circular with K from the circular formula; if real binary masses vary between surveys, the two q3 peaks and the identification of the low-q3 peak with old Bulge systems would not be reliable.

Editorial extensions

If this is right

The low-q3 peak (0.2-0.35) in the combined sample is dominated by OGLE Bulge systems, identifying them as old CHTs, while the near-unity q3 peak from Gaia and Kepler identifies younger systems.
The cumulative e2 distribution lies above a flat distribution at all eccentricities, so CHT outer orbits are dynamically excited beyond what random formation would produce.
Survey-to-survey differences in the low-eccentricity part of the e2 distribution track metallicity, with the Kepler sample apparently metal-poor.
Because stellar evolution cannot provide enough mass loss to move q3 from unity to about 0.2, tidal dissipation or circumbinary disk interactions must be acting, and this also explains the planar CHT population.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

The mbin = 2 solar masses assumption is strong: if the true inner binary masses in the OGLE sample are systematically lower, the low-q3 peak would shift; measuring masses directly for a subset is a natural next step the paper itself calls for.
The low-q3 OGLE peak may be partly a selection effect of ETV surveys, which are less sensitive to low-mass tertiaries; completeness corrections could change the bimodality's height even if not its existence.
The inferred metallicity-eccentricity connection would be directly testable by measuring spectroscopic metallicities of Gaia CHTs, which currently enter only through the eccentricity-shape comparison.
With future mutual-inclination measurements, the tidal-dissipation versus circumbinary-disk-mass-loss mechanisms for shifting q3 could be distinguished.

Share X Bluesky LinkedIn Reddit HN

Signed reviews

No signed human review yet.

Editorial analysis

A structured set of objections, weighed in public.

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

Desk Editor's Note

read the letter

Short version: this is an honest, exploratory conference paper that brings together the GAIA-NSS, OGLE, and Kepler CHT samples and points out survey-to-survey differences in the e2 and q3 distributions. That joint presentation is genuinely new, and the cross-survey eccentricity comparison (Kepler sub-flat at low e2, OGLE intermediate behavior) is a real observation I haven't seen stated before. The OGLE dominance of the low-q3 peak is also new. The paper deserves credit for being transparent: it labels the q3 estimates 'ad-hoc' and says the calculations are approximate.

But the central interpretation—that the q3 bimodality traces age and the e2 shape traces metallicity—is not actually supported by the data as presented. The load-bearing assumption is a fixed inner-binary mass of 2 Msun for every system. Since q3 scales roughly as (f/mbin)^(1/3), a factor-of-two mass difference between surveys shifts q3 by 20-25%. If the typical OGLE Bulge inner binary is less massive than 2 Msun and the typical GAIA host is more massive, the fixed assumption pushes OGLE q3 down and GAIA q3 up, creating or strongly enhancing the very bimodality attributed to age. The GAIA values are also derived with e2=0 and K=2πa2/P2, so the two catalogs are not on the same physical footing. And the population labels (old vs young, metal-poor vs metal-rich) are imported from the authors' own earlier work and applied to the new samples without independent age or metallicity measurements. Finally, there are no error bars or significance tests anywhere; the bimodality and the sub-flat features are read off histograms. The paper itself admits the q3 estimates are approximate, so it isn't overclaiming, but the main conclusion is a hypothesis, not a measurement.

This is a conference proceedings, so the length constraints may explain some of the shortcuts. Still, the central claim could be tested cheaply: propagate a plausible range of mbin across surveys and see if the bimodality survives. That should have been done before submitting.

Who is this for? People working on stellar multiplicity and triple formation who want a quick combined view of the current CHT samples. It deserves a serious referee rather than a desk reject, because it makes a concrete, falsifiable claim about formation channels and survey differences, and the underlying data are public. Recommendation: send to peer review, require the authors to test the mbin sensitivity, add at least basic bootstrap uncertainties, and tone down the age/metallicity interpretation unless they bring in external data.

Referee Report

3 major / 5 minor

Summary. The paper analyzes orbital parameters of compact hierarchical triples (CHTs) from Kepler, OGLE, and Gaia DR3 NSS catalogs. It constructs distributions of tertiary eccentricity e2 and tertiary-to-inner-binary mass ratio q3, arguing that the e2 distribution shows survey-dependent trends attributable to metallicity and that the q3 distribution is bimodal, with a low-q3 peak dominated by old OGLE Bulge systems and a high-q3 peak from younger systems. These demographic features are interpreted as signatures of sequential disk-instability (DI+DI) formation, supplemented by tidal dissipation. The central empirical claims are the survey-decomposed e2 and q3 distributions in Figs. 2 and 3.

Significance. If the claims hold, the paper would provide an observationally grounded link between the formation mechanism of compact hierarchical triples and the demographic differences between Galactic populations, which is a valuable contribution given the recent growth of CHT catalogs. The paper draws on large, publicly available samples (110 Kepler CHTs, 177 OGLE CHTs, and 376 Gaia CHT candidates) and explicitly labels the approximations in the mass-ratio derivation. However, the central demographic conclusions rest on a single assumed inner-binary mass for all systems, on a simplified treatment of Gaia orbits, and on visual comparisons without statistical uncertainties. These limitations directly affect the bimodality and metallicity interpretations, so the significance of the results is conditional on addressing them.

major comments (3)

[Sec. 3, Eqs. (2)-(4)] The q3 distribution is constructed by assuming a single inner-binary mass, mbin = 2 Msun, for every system, and for Gaia systems by additionally setting e2 = 0 and approximating K as 2*pi*a2/P2. This is load-bearing because Eq. (2) maps the mass function to q3 nonlinearly; for q3 < 1, q3 scales approximately as (f/mbin)^(1/3), so a factor-of-two difference in the assumed mbin shifts q3 by roughly 20-25%. The low-q3 peak in Fig. 3 is dominated by the OGLE Bulge sample and the high-q3 peak by the Gaia sample, so if typical Bulge OGLE inner binaries are less massive than 2 Msun while typical Gaia hosts are more massive, the fixed assumption would systematically skew OGLE q3 downward and Gaia q3 upward, potentially creating or strongly enhancing the very bimodality that is interpreted as an age effect. The paper should either justify mbin per survey with empirical mass distributions, propagate a range of plausible mbin values, or explicitly show that the bimodality persists under such variations.
[Sec. 4.2, Fig. 3 and Sec. 4.1, Fig. 2] The claims of bimodality in q3 and of survey-dependent differences in e2 are based on visual inspection of histograms and cumulative distributions, with no error bars, bootstrap resampling, or significance tests. The sample sizes differ strongly across surveys (e.g., 177 OGLE systems vs. 45 robust Kepler solutions), so Poisson fluctuations and sample-selection effects could produce apparent structure that is not physical. At minimum, the authors should provide per-bin uncertainties and a statistical test (e.g., a bootstrap or a two-sample test) to assess whether the two q3 peaks are distinguishable and whether the e2 sub-flat trends are significant.
[Sec. 4.1 and Sec. 4.2] The interpretation of the sub-flat e2 trend at e2 = 0.1-0.25 as indicating metal-poor CHTs, and the interpretation of the q3 bimodality as reflecting old versus young populations, are taken from the authors' own Moharana et al. (2024) and then applied to label the Kepler, OGLE, and Gaia samples without independent metallicity or age estimates for the present sample. This creates a circularity risk: the same calibration is used to interpret the new data and to support the formation scenario. The paper should either obtain or cite direct metallicity and age measurements for the individual systems, or clearly reframe these as tentative hypotheses rather than derived conclusions.

minor comments (5)

[Author list] The author name "K.G. He/suppress lminiak" appears garbled; this should be corrected (presumably to K.G. Hełminiak).
[Abstract] The abstract contains received and accepted dates (May 1, 2020; July 28, 2020) that are inconsistent with the November 2024 submission date; these should be removed or updated.
[Introduction] There is a grammatical error in the sentence "This percentage increases are we go towards high-mass stars," which should read "This percentage increases as we go towards high-mass stars."
[Sec. 4.3, last paragraph] The statement "our calculations are approximate and do not precisely estimate the q3" is important caveat; it should be stated earlier, at the point where the q3 distribution is introduced (Sec. 4.2), so that readers are not misled by the apparent precision of the histograms in Fig. 3.
[Fig. 1] The period distribution in Fig. 1 would benefit from a legend or explicit labeling of which histogram corresponds to which survey, as the current gray-scale differentiation is difficult to interpret.

Circularity Check

0 steps flagged · score 0.0 of 10

No circular reduction found: the q3 and e2 distributions are derived from external catalogs, the fixed mbin=2 Msun assumption is an acknowledged approximation rather than a fitted input, and the interpretive self-citations are to prior independent spectroscopic work.

full rationale

The paper's derivation chain for q3 is: the tertiary mass function f is taken from ETV surveys (Borkovits 2016; Hajdu 2019) or approximated for GAIA via Eqs. (3)-(4), and then q3 is obtained by solving Eq. (2) under the stated assumption mbin = 2 Msun. This is an approximate conversion of observed orbital parameters, not a parameter fitted to reproduce the target distribution, so the resulting bimodality is not a circular prediction. The e2 and q3 distributions are computed from external Kepler, OGLE, and GAIA-NSS catalogs, giving the core comparison independent content. The interpretive steps in Secs. 4.1 and 4.2 cite Moharana et al. (2024) for the metallicity dependence of the sub-flat e2 trend and for the age dependence of the q3 bimodality; that prior work is a separate spectroscopic study, and the present paper does not define its target conclusion in terms of that citation. Without evidence that the cited result is itself built on the same fixed-mbin assumption or on the present claim, these are cumulative empirical references rather than a by-construction reduction. The paper explicitly admits the q3 calculations are approximate (Sec. 4.3), and the skeptic's concern that survey-dependent mbin values could shift the q3 peaks is a robustness/correctness issue, not a logical circularity. No equation-level or definitional reduction is exhibited, so the circularity score is 0.

Assumptions & free parameters 3 free parameters · 4 assumptions · 0 invented entities

The paper's central inferences depend on an assumed inner binary mass, a circular-orbit approximation for Gaia targets, the representativeness of three external catalogs, and empirical age or metallicity links from the authors' prior paper. No new data or code are provided; the mass-ratio distribution is explicitly called ad-hoc.

free parameters (3)

mbin = 2 M_sun
Assumed total inner binary mass for all systems when solving the cubic for q3 (Sec. 3: 'assuming mbin = 2 M_sun'). The derived mass-ratio distribution and its bimodality depend on this choice.
e2 (GAIA) = 0
Outer eccentricity set to zero in Eq. 4 when deriving fGAIA from a2 and P2, although the paper later analyzes the e2 distribution (Sec. 3).
K approximation = K = 2*pi*a2/P2
For GAIA-NSS targets the RV semi-amplitude K is not available, so K is approximated as the circular velocity of the outer orbit (Sec. 3, Eq. 3), which feeds into the mass function and q3.

assumptions (4)

standard math Kepler's third law and the mass-function equation (Eq. 1) relate observed P2, K, e2 to m3 and mbin.
Used in Sec. 3 to transform orbital parameters into mass ratios; standard celestial mechanics.
domain assumption The Gaia DR3 non-single-star orbital solutions correspond to the outer tertiary orbits in these CHTs.
Assumed after crossmatching with EB catalogs (Sec. 2, citing Czavalinga et al. 2023); if some solutions are inner orbits or spurious, the derived q3 distribution is wrong.
domain assumption The selected samples (45 robust Kepler, 177 robust OGLE, roughly 376 Gaia crossmatches) are representative of the CHT population and selection effects do not dominate the distributions.
Sec. 2 selects robust solutions from literature; the paper does not model detection biases or completeness.
domain assumption The empirical link that metal-poor CHTs show sub-flat e2 at 0.1 to 0.25 and that young or old CHTs have different q3 from Moharana et al. (2024) applies to the new combined samples.
Invoked in Sec. 4.1-4.2 to label Kepler as metal-poor and OGLE as old; the underlying evidence is a self-cited prior paper.

how reviews work

0 comments

Cite this review

Pith. "Pith review of Formation of Compact Hierarchical Triples." pith.science (2026). https://pith.science/paper/Z6HSRXZE

@misc{pith2026241111459,
  author       = {Pith},
  title        = {Pith review of: Formation of Compact Hierarchical Triples},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/Z6HSRXZE}},
  note         = {Machine review of arXiv:2411.11459}
}

read the original abstract

Compact hierarchical triples (CHTs) are triple stars where the tertiary is in an orbit of a period less than 1000 d. They were thought to be rare but we are discovering more of these systems recently, thanks to space-based missions like TESS, Kepler, and GAIA. In this work, we use orbital parameters obtained from these missions to constrain the formation process of CHTs. We also use spectroscopic and systemic parameters from our work, and the literature to understand the effects of metallicity and dynamics on the formation processes.

Figures

Figures reproduced from arXiv: 2411.11459 by the authors.

**Figure 1.** Distribution of orbital periods for the sample of CHTs used in this work. The grey lines mark the stability limits. The horizontal line on the left part of the plot represents the period limit for contact binaries while the slanted line on the right represents the limit for dynamical stability. for f is K. For our approximation, we set K = 2πa2/P2 (3) where a2 is available from GAIA-NSS solutions. From Eq.1 and taki… view at source ↗

**Figure 2.** Cumulative probability distribution of e2 for the sample of CHTs. The sub- -samples of GAIA-NSS, OGLE, and Kepler are represented by grey-solid, grey-dashed, and black-solid lines respectively. The slanted grey line represents the expected trend for a flat distribution. 4.2. Bi-modality in mass ratio distribution One of the expected outcomes of the DI+DI scenario of star formation is that it produces “twins”, meanin… view at source ↗

**Figure 3.** Distribution of q3 for the large sample of CHTs (shaded histogram). The sub-samples of GAIA-NSS, OGLE, and Kepler are represented by grey-solid, grey– dashed, and black-solid lines respectively. 4.3. Dynamical processes and time evolution of distributions The distributions of e2 and q3 are consistent with the DI+DI formation scenario but there is also a need to account for the additional dynamical processes that exi… view at source ↗

Discussion (0). Continue with ORCID to comment.

Forward citations

Cited by 1 Pith paper

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

Eccentricities of Close Stellar Binaries
astro-ph.SR 2024-11 conditional novelty 8.0 of 10

Close stellar binaries in the AU-scale range have eccentricities distributed as a Rayleigh distribution with mode σ_e ≈ 0.3, likely primordial and universal.

Reference graph

Works this paper leans on

13 extracted references · 1 linked inside Pith · cited by 1 Pith paper

[1]

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

ENTRY address archiveprefix author booktitle chapter edition editor howpublished institution eprint journal key month note number organization pages publisher school series title type volume year doi label extra.label sort.label short.list INTEGERS output.state before.all mid.sentence after.sentence after.block FUNCTION init.state.consts #0 'before.all :=...
[2]

write newline

" write newline "" before.all 'output.state := FUNCTION n.dashify 't := "" t empty not t #1 #1 substring "-" = t #1 #2 substring "--" = not "--" * t #2 global.max substring 't := t #1 #1 substring "-" = "-" * t #2 global.max substring 't := while if t #1 #1 substring * t #2 global.max substring 't := if while FUNCTION word.in bbl.in " " * FUNCTION format....
[3]

2022, Galaxies , 10 , 9, DOI: 10.3390/galaxies10010009

Borkovits , T., Eclipsing Binaries in Dynamically Interacting Close, Multiple Systems . 2022, Galaxies , 10 , 9, DOI: 10.3390/galaxies10010009

doi:10.3390/galaxies10010009 2022
[4]

, A comprehensive study of the Kepler triples via eclipse timing

Borkovits , T., Hajdu , T., Sztakovics , J., et al. , A comprehensive study of the Kepler triples via eclipse timing . 2016, , 455 , 4136, DOI: 10.1093/mnras/stv2530

doi:10.1093/mnras/stv2530 2016
[5]

A., Toonen , S., et al

Borkovits , T., Rappaport , S. A., Toonen , S., et al. , Von Zeipel - Lidov - Kozai cycles in action: Kepler triples with eclipse depth variations: KICs 6964043, 5653126, 5731312, and 8023317 . 2022, , 515 , 3773, DOI: 10.1093/mnras/stac1983

doi:10.1093/mnras/stac1983 2022
[6]

R., Mitnyan , T., Rappaport , S

Czavalinga , D. R., Mitnyan , T., Rappaport , S. A., et al. , New compact hierarchical triple system candidates identified using Gaia DR3 . 2023, , 670 , A75, DOI: 10.1051/0004-6361/202245300

doi:10.1051/0004-6361/202245300 2023
[7]

L., Johnston , C., Toonen , S., et al

Eisner , N. L., Johnston , C., Toonen , S., et al. , Planet Hunters TESS IV: a massive, compact hierarchical triple star system TIC 470710327 . 2022, , 511 , 4710, DOI: 10.1093/mnras/stab3619

doi:10.1093/mnras/stab3619 2022
[8]

, Gaia Data Release 3

Gaia Collaboration , Arenou , F., Babusiaux , C., et al. , Gaia Data Release 3. Stellar multiplicity, a teaser for the hidden treasure . 2023, , 674 , A34, DOI: 10.1051/0004-6361/202243782

doi:10.1051/0004-6361/202243782 2023

Show all 13 references

[9]

, Eclipse timing variation analysis of OGLE-IV eclipsing binaries towards the Galactic Bulge - I

Hajdu , T., Borkovits , T., Forg \'a cs-Dajka , E., et al. , Eclipse timing variation analysis of OGLE-IV eclipsing binaries towards the Galactic Bulge - I. Hierarchical triple system candidates . 2019, , 485 , 2562, DOI: 10.1093/mnras/stz592

2019 doi
[10]

G., Marcadon , F., et al

Moharana , A., He miniak , K. G., Marcadon , F., et al. , Spectroscopy of eclipsing compact hierarchical triples: I. Low-mass double-lined and triple-lined systems . 2024, , 690 , A153, DOI: 10.1051/0004-6361/202450797

2024 doi
[11]

A., Henry , T

Raghavan , D., McAlister , H. A., Henry , T. J., et al. , A Survey of Stellar Families: Multiplicity of Solar-type Stars . 2010, , 190 , 1, DOI: 10.1088/0067-0049/190/1/1

2010 doi
[12]

, The OGLE Collection of Variable Stars

Soszy \'n ski , I., Pawlak , M., Pietrukowicz , P., et al. , The OGLE Collection of Variable Stars. Over 450 000 Eclipsing and Ellipsoidal Binary Systems Toward the Galactic Bulge . 2016, , 66 , 405, DOI: 10.48550/arXiv.1701.03105

2016 doi arXiv
[13]

2017, , 844 , 103, DOI: 10.3847/1538-4357/aa7746

Tokovinin , A., Orbit Alignment in Triple Stars . 2017, , 844 , 103, DOI: 10.3847/1538-4357/aa7746

2017 doi

Pith tools

Reviewed August 12, 2026 · model on record in the stance chip above.

[1] [1]

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

ENTRY address archiveprefix author booktitle chapter edition editor howpublished institution eprint journal key month note number organization pages publisher school series title type volume year doi label extra.label sort.label short.list INTEGERS output.state before.all mid.sentence after.sentence after.block FUNCTION init.state.consts #0 'before.all :=...

[2] [2]

write newline

" write newline "" before.all 'output.state := FUNCTION n.dashify 't := "" t empty not t #1 #1 substring "-" = t #1 #2 substring "--" = not "--" * t #2 global.max substring 't := t #1 #1 substring "-" = "-" * t #2 global.max substring 't := while if t #1 #1 substring * t #2 global.max substring 't := if while FUNCTION word.in bbl.in " " * FUNCTION format....

[3] [3]

2022, Galaxies , 10 , 9, DOI: 10.3390/galaxies10010009

Borkovits , T., Eclipsing Binaries in Dynamically Interacting Close, Multiple Systems . 2022, Galaxies , 10 , 9, DOI: 10.3390/galaxies10010009

doi:10.3390/galaxies10010009 2022

[4] [4]

, A comprehensive study of the Kepler triples via eclipse timing

Borkovits , T., Hajdu , T., Sztakovics , J., et al. , A comprehensive study of the Kepler triples via eclipse timing . 2016, , 455 , 4136, DOI: 10.1093/mnras/stv2530

doi:10.1093/mnras/stv2530 2016

[5] [5]

A., Toonen , S., et al

Borkovits , T., Rappaport , S. A., Toonen , S., et al. , Von Zeipel - Lidov - Kozai cycles in action: Kepler triples with eclipse depth variations: KICs 6964043, 5653126, 5731312, and 8023317 . 2022, , 515 , 3773, DOI: 10.1093/mnras/stac1983

doi:10.1093/mnras/stac1983 2022

[6] [6]

R., Mitnyan , T., Rappaport , S

Czavalinga , D. R., Mitnyan , T., Rappaport , S. A., et al. , New compact hierarchical triple system candidates identified using Gaia DR3 . 2023, , 670 , A75, DOI: 10.1051/0004-6361/202245300

doi:10.1051/0004-6361/202245300 2023

[7] [7]

L., Johnston , C., Toonen , S., et al

Eisner , N. L., Johnston , C., Toonen , S., et al. , Planet Hunters TESS IV: a massive, compact hierarchical triple star system TIC 470710327 . 2022, , 511 , 4710, DOI: 10.1093/mnras/stab3619

doi:10.1093/mnras/stab3619 2022

[8] [8]

, Gaia Data Release 3

Gaia Collaboration , Arenou , F., Babusiaux , C., et al. , Gaia Data Release 3. Stellar multiplicity, a teaser for the hidden treasure . 2023, , 674 , A34, DOI: 10.1051/0004-6361/202243782

doi:10.1051/0004-6361/202243782 2023