Pith. sign in

REVIEW 3 major objections 7 minor 34 references

Gaia DR2 white dwarfs in the Hercules stream

T0 review · 3 major / 7 minor · reviewed 2026-08-14 · deepseek-v4-flash

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

Pith's one-line read The paper claims that the Hercules stream, a kinematic overdensity previously seen in main-sequence stars, is present in the Gaia white dwarf population within 100 pc, with three substreams whose ages favor a dynamical origin.

desk verdict First white-dwarf detection of the Hercules stream and a first age distribution, but the zero-RV assumption, small clusters, and missing error bars make the substructure and age peaks provisional. read the letter →

arxiv 1908.02972 v1 pith:ZFLK3XLI submitted 2019-08-08 astro-ph.SR astro-ph.GA

Santiago Torres , Carles Cantero , María E. Camisassa , Teresa Antoja , Alberto Rebassa-Mansergas , Leandro G. Althaus , Thomas Thelemaque , Héctor Cánovas This is my paper · ORCID
classification astro-ph.SRastro-ph.GA
keywords whitedwarfsHerculesstreamGalactickinematicssolarneighborhoodGaiaDR2thickdiskHDBSCANdwarfages
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

This paper argues that the Hercules stream, a well-known kinematic overdensity in the solar neighborhood, is present among the white dwarfs within 100 pc. A kernel-density analysis of the $UV$ velocity plane of the thick-disk white dwarf population reveals an overdensity centered at $(U,V)=(-55,-50)$ km/s with roughly three times the average density; no such feature appears in the thin disk. Applying the HDBSCAN clustering algorithm to a five-dimensional dynamical space, the authors identify three substreams, Her a, Her b, and Her c, whose positions match earlier detections of Hercules substructure. Using white dwarfs as cosmochronometers, they estimate that Her a and Her b are predominantly thick-disk stars with ages peaking near 4 Gyr, while Her c is a 65:35 thin:thick mix with a more uniform distribution below 10 Gyr. The finding matters because it extends the stream to a new tracer population and gives a first age handle on its members.

What carries the argument

The argument is carried by three tools. First, a nearly complete, volume-limited sample of Gaia white dwarfs within 100 pc, classified into thin-disk and thick-disk populations by a random-forest algorithm, provides the kinematic canvas. Second, the Hercules signature is isolated by kernel density estimation in the $UV$ velocity plane and then by HDBSCAN, a hierarchical density-based clustering algorithm, applied to a five-dimensional space of dynamical variables: $U$, $V$, the peculiar speed $V_{\mathrm{pec}}=(U^2+V^2+W^2)^{1/2}$, the Toomre velocity $V_{\mathrm{Toomre}}=(U^2+W^2)^{1/2}$, and $V_{\Delta E}=(U^2+2V^2)^{1/2}$, which is proportional to the square root of orbital eccentricity. Third, the ages come from matching Gaia absolute magnitudes and colors to white dwarf cooling sequences with hydrogen-rich atmospheres and metallicities $Z=0.01$ (thin disk) and $Z=0.001$ (thick disk); the total age is the cooling time plus the progenitor main-sequence lifetime, and objects below $0.53\,M_{\odot}$ are excluded as probable binary remnants.

What would settle it

Take spectra of the 57 white dwarfs assigned to Her a, Her b, and Her c, measure their radial velocities, recompute the full $(U,V,W)$ velocities, and rerun the kernel density estimation and HDBSCAN clustering. If the overdensity at $(U,V)=(-55,-50)$ km/s vanishes, or the three groups shift by more than their internal velocity dispersions (roughly 2–3 km/s) or change membership, the claimed substreams depend on the zero-radial-velocity assumption rather than on a real Galactic stream.

Watch

Extended reading notes

Core claim

The central discovery is that the Hercules stream signature is visible in the kinematics of the Gaia DR2 white dwarf population within 100 pc. In the thick-disk subsample, kernel density estimation in the $(U,V)$ plane reveals an overdensity centered at $(U,V)=(-55,-50)\,\mathrm{km\,s^{-1}}$, spanning $(\Delta U,\Delta V)=(60,50)\,\mathrm{km\,s^{-1}}$ and containing roughly three times the average number density per $(\mathrm{km\,s^{-1}})^2$; in the same region 68% of the thick-disk white dwarfs have negative $U$. The authors then run HDBSCAN on a normalized five-dimensional space of dynamical variables and recover three compact groups: Her a (19 objects at $(-58.5,-54.7)$), Her b (18 objects at $(-69.3,-41.4)$), and Her c (20 objects at $(-29.9,-50.7)$), matching the previously known Hercules I/II and A8/A9 substructures. Her a is entirely thick-disk, Her b all but one thick-disk, and Her c is 65% thin-disk and 35% thick-disk. Photometric ages from white dwarf cooling sequences give a peak near 4 Gyr for Her a and b with tails to very old ages, while Her c is more uniform between 2 and 10 Gyr. The paper concludes that the Hercules stream is present in the white dwarf population and that the extended ages favor a dynamical origin for the stream over cluster disruption.

Load-bearing premise

The load-bearing premise is that assuming a zero radial velocity for every white dwarf—because these objects lack such measurements—does not create or distort the Hercules overdensity and its three substreams; the paper's own Monte Carlo estimate says the resulting shifts in $(U,V)$ are of the order of a few to tens of km/s, comparable to the separations between the claimed groups.

Editorial extensions

If this is right

  • The Hercules stream can now be traced with white dwarfs, giving an independent, volume-complete sample of stream members that does not rely on main-sequence color-magnitude selection.
  • The age estimates give the first age constraint on stream members: Her a and b peaked roughly 4 Gyr ago and extend to very old ages, while Her c is younger and more uniform, so any formation model must reproduce this age structure.
  • The presence of Hercules-like kinematic structure in the thick disk is consistent with bar-resonance models that perturb the thick disk as well as the thin disk, supporting the dynamical-origin interpretation over cluster disruption.
  • The three substreams correspond to the previously identified Hercules I/II and A8/A9 structures, confirming that the substructure appears in an independent tracer.

Reading between the lines

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

  • If the zero-radial-velocity assumption shifts stream members' $U,V$ positions in a correlated way, the separation between Her a, b, and c could be partly an artifact: the paper's quoted systematic shifts are comparable to the inter-substream separations, so a targeted radial-velocity campaign is the decisive test.
  • The same five-dimensional HDBSCAN strategy could be applied to the halo white dwarfs or to larger samples beyond 100 pc in future Gaia releases, potentially uncovering other moving groups among stellar remnants.
  • Combining the estimated ages with orbit integrations in a barred potential could test whether stars of a given age were trapped at the relevant resonance at a particular time, connecting the stream's 4 Gyr peak to the bar's pattern speed.
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.

Referee Report

3 major / 7 minor

Summary. The paper analyzes the velocity space of a nearly volume-limited 100 pc sample of Gaia DR2 white dwarf candidates, separated into thin-disk, thick-disk, and halo populations using the authors' earlier Random Forest classification. Heliocentric (U,V) velocities are computed from Gaia astrometry under the assumption that every white dwarf has zero radial velocity. A kernel density estimate of the thick-disk UV plane reveals an overdensity near (U,V)=(-55,-50) km/s with a claimed density about three times the average, which the authors identify with the Hercules stream. Restricting to this overdensity rectangle, the authors apply HDBSCAN to a 5D kinematic space and identify three groups of roughly 18-20 stars each (Her a, Her b, Her c), whose (U,V) positions are compared with previously published Hercules substructures. Using photometric cooling models, they derive age distributions: Her a and Her b are predominantly thick-disk with ages peaking near 4 Gyr, while Her c is 65% thin-disk and 35% thick-disk with a flatter age distribution. The paper concludes that the Hercules stream signature is present in the white dwarf population and provides first age estimates.

Significance. If the detection holds, the result is valuable: it extends a well-studied kinematic stream to a new tracer population, exploits a nearly complete census of white dwarfs in the solar neighborhood, and offers an age distribution that is plausibly consistent with a dynamical, bar-related origin rather than cluster disruption. The external anchor to previously published Hercules positions from Antoja et al. (2012) and Ramos et al. (2018) is a genuine strength and reduces concern that the identification is circular. The paper is also transparent about its assumptions, particularly the lack of radial velocities. However, the central detection currently rests on a zero-radial-velocity assumption whose defense is insufficient, and the substructure and age claims rely on small clusters whose robustness is not demonstrated. These issues are load-bearing and need to be addressed before the result can be considered established.

major comments (3)
  1. [Secs. 2-3] The defense against the zero-radial-velocity assumption is not sufficient for the claim being made. The quoted Monte Carlo results from Torres et al. (2019) report only mean reductions of the (U,V) components, with standard deviations of 17-32 km/s; they do not test whether applying the zero-RV projection to a smooth thick-disk velocity ellipsoid can create a localized overdensity of roughly three times the average density at (U,V)=(-55,-50) km/s. The detection statistic is the overdensity itself, not a global asymmetry, so the statement that the zero-RV effect 'does not generate any asymmetry' is not responsive. I request a dedicated null test: draw a smooth model of the thick-disk velocity distribution, apply the same astrometric projection with zero radial velocities, and verify that no comparable overdensity appears at the Hercules location. This is essential because the reported dispersions are comparable to the separation between Her a and Her b (about 17 km/s), meaning the substructure grouping could also be distorted by the assumption.
  2. [Sec. 3 and Fig. 1] The significance of the overdensity is not quantified. The text says the red rectangle region has a number of objects per (km/s)^2 'roughly 3 times larger than the average density,' but no uncertainty or significance is given. With only 1,410 thick-disk candidates and roughly 20 stars per claimed substructure, one needs a Poisson or bootstrap estimate of the overdensity significance, plus a statement of how many stars fall in the red rectangle versus the number expected from a smooth fit to the surrounding velocity distribution. The incompleteness/croissant-shape discussion is qualitative and does not replace this quantitative test.
  3. [Sec. 3, HDBSCAN application] The clustering step is not validated against false positives. HDBSCAN is applied with mPts in the range 10-30 and membership probability larger than 90%, and the three substreams contain only 18-20 stars each. No stability analysis is presented: the authors do not show how the number and positions of clusters vary with mPts, do not bootstrap the sample, and do not run the same pipeline on a smooth synthetic UV distribution to see how often HDBSCAN returns comparable clusters by chance. Because HDBSCAN is designed to find clusters in arbitrary density fields, the separation of Her a and Her b into distinct substreams, and the subsequent age differences, are not yet robust. I recommend a permutation or mock-catalog test with the same sample size and selection function.
minor comments (7)
  1. [Abstract] The word 'hierarchichal' should be 'hierarchical.'
  2. [Sec. 3] The 'croissant-shape' of the thick-disk distribution is mentioned but not defined or illustrated; please add a brief explanation or a reference where this shape is described.
  3. [Table 1] The claim of 'excellent agreement' with literature substructures should be quantified. Some of the literature positions have no quoted uncertainties, and offsets of 10-20 km/s are comparable to the separations between the newly claimed substreams, so visual agreement alone is not a strong test.
  4. [Fig. 2] The legend uses 'blue circles' for Her a and 'cyan circles' for Her c; these colors may be difficult to distinguish in print. Please use distinct symbols or more separated colors.
  5. [Sec. 4] The K-S test paragraph appears to contain an inconsistency: the text says Her a and Her c are consistent with a normal distribution, but then says 'the age distribution of Her c is unlikely normally distributed.' This likely should refer to Her a and Her b, or Her b and Her c; please correct.
  6. [Sec. 3] The list of white dwarfs in each substream is said to be 'available upon request'; for reproducibility and because the member list is a central product, please include it as a machine-readable table or in an appendix.
  7. [Conclusions] 'firstly revealed' should be 'first revealed' in the abstract and conclusions.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the Hercules overdensity and substreams are measured from Gaia data and validated against external catalogs; self-citations are independent prior work.

full rationale

The paper's derivation chain is self-contained and contains no step that reduces to its own inputs by construction. The central detection is a KDE overdensity measured from Gaia DR2 astrometry for the thick-disk white dwarf sample; the overdensity location and the HDBSCAN clusters (Her a/b/c) are outputs of the data and of an unsupervised clustering algorithm on a 5-D kinematic space, not parameters fitted to reproduce the literature positions of Hercules. Validation against Antoja et al. (2012), Bobylev & Bajkova (2016), and Ramos et al. (2018) is post-hoc. The ages are computed from photometry and published cooling tracks after cluster membership is fixed, so they cannot feed back into the clustering. The zero-radial-velocity concern is a possible correctness risk, but the paper's rebuttal cites Torres et al. (2019), a prior Monte Carlo control that does not include the Hercules overdensity as an input; citing one's own earlier external control does not make the detection definitionally circular. The same applies to the thin/thick-disk classification and the cooling tracks. No equation in the paper equates a fitted parameter with a claimed prediction, and no uniqueness or ansatz is imported from a self-citation to force the substream identification.

Assumptions & free parameters 4 free parameters · 6 assumptions · 0 invented entities

The paper's central results rest on a series of assumptions: zero radial velocities for white dwarfs, the machine-learning disk classification from the authors' own prior work, adopted (not measured) metallicities and DA atmospheres, a flat rotation curve for the eccentricity proxy, and theoretical cooling models. None of these are fitted in this paper, but they are all external inputs whose errors propagate into the substream identification and age distributions.

free parameters (4)
  • HDBSCAN mPts = 10-30, exact value not stated
    Minimum number of objects to form a cluster; chosen by the authors in a range, not specified precisely, and it controls the number and membership of clusters (Sec. 3).
  • HDBSCAN cluster membership probability threshold = >90%
    Threshold used to assign white dwarfs to clusters; chosen by the authors without a principled justification (Sec. 3).
  • KDE bandwidth = not stated
    The kernel density estimation used to reveal the UV-plane overdensity requires a bandwidth choice, but no value or method is reported (Sec. 3).
  • Overdensity selection box = centered (U,V)=(-55,-50), size (60,50) km/s
    The red rectangle in Fig. 1 is chosen by eye around the overdensity; the clustering is applied only inside it, so the box definition affects which stars are considered (Sec. 3).
assumptions (6)
  • domain assumption Radial velocity is zero for every white dwarf
    Used in Sec. 2 to compute heliocentric (U,V,W) velocities from proper motions and parallaxes, since WDs lack RV measurements; the paper argues via Monte Carlo that this does not create the overdensity.
  • domain assumption Thin/thick-disk classification of Torres et al. (2019) is accurate
    The sample is split into thin and thick disk using a Random Forest classifier from the same group (Torres et al. 2019). The overdensity is only claimed in the thick-disk population, so classification errors could create or remove the feature.
  • domain assumption All white dwarfs in the sample have hydrogen-rich (DA) atmospheres
    Assumed in Sec. 4 to convert photometry to ages; no spectroscopy is available, and a fraction of WDs are helium-rich (DB), which would change the derived ages.
  • domain assumption Thin-disk WDs have Z=0.01 and thick-disk WDs have Z=0.001
    Adopted in Sec. 4 for age estimation; the paper states a small dispersion is expected and has negligible effect after 1 Gyr binning, but this is not demonstrated.
  • domain assumption V_DeltaE = sqrt(U^2+2V^2) is a valid eccentricity proxy based on a flat rotation curve
    Used in Sec. 3 as one of the 5-D clustering variables; if the rotation curve is not flat, this variable is not the stated eccentricity proxy.
  • domain assumption Cooling tracks and initial-final mass relations of Althaus et al. (2015) and Camisassa et al. (2016, 2018) are accurate
    Used in Sec. 4 to convert MG and GBP-GRP to total ages; systematic errors in the models translate directly into age errors.

how reviews work

0 comments
Cite this review

Pith. "Pith review of Gaia DR2 white dwarfs in the Hercules stream." pith.science (2026). https://pith.science/paper/ZFLK3XLI

@misc{pith2026190802972,
  author       = {Pith},
  title        = {Pith review of: Gaia DR2 white dwarfs in the Hercules stream},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/ZFLK3XLI}},
  note         = {Machine review of arXiv:1908.02972}
}
abstract

We analyzed the velocity space of the thin and thick-disk Gaia white dwarf population within 100 pc looking for signatures of the Hercules stellar stream. We aimed to identify those objects belonging to the Hercules stream and, by taking advantage of white dwarf stars as reliable cosmochronometers, to derive a first age distribution. We applied a kernel density estimation to the $UV$ velocity space of white dwarfs. For the region where a clear overdensity of stars was found, we created a 5-D space of dynamic variables. We applied a hierarchichal clustering method, HDBSCAN, to this 5-D space, identifying those white dwarfs that share similar kinematic characteristics. Finally, under general assumptions and from their photometric properties, we derived an age estimate for each object. The Hercules stream was firstly revealed as an overdensity in the $UV$ velocity space of the thick-disk white dwarf population. Three substreams were then found: Hercules $a$ and Hercules $b$, formed by thick-disk stars with an age distribution peaked $4\,$Gyr in the past and extended to very old ages; and Hercules $c$, with a ratio of 65:35 thin:thick stars and a more uniform age distribution younger than 10 Gyr.

Figures

Figures reproduced from arXiv: 1908.02972 by the authors.

Figure 1
Figure 1. UV density diagram for the thin (top panel) and thick-disk (bot￾tom panel) white dwarf population within 100 pc from the Sun. A clear overdensity is revealed in the thick-disk population (delimited by a red rectangle). For comparative purposes, we show the thin-disk dis￾persion ellipsoid for 1σ (continuous line) and 3σ (dashed line) lev￾els corresponding to the thin-disk population (Torres et al. 2019) and we illust… view at source ↗
Figure 2
Figure 2. UV diagram (left panel) and Toomre diagram (right panel) for the thin and thick-disk white dwarf population (black and red dots, respec￾tively, and color emphasized those belonging to the selected overdensity region). Also plotted are the structures Her a (blue circles), Her b (blue triangles) and Her c (cyan circles) found in this work . For comparative purposes, we show as yellow squares the locations in the UV pl… view at source ↗
Figure 3
Figure 3. Age distribution for each of the three Hercules sub-stream identified in this work and for all of them considered together (right panel). The sub-stream Her b presents a maximum at around 4 Gyr with an extended long tail up to very old ages. Her a is similar, but with a less clear peak. Sub-stream Her c appears as a more uniform distribution between 2 and 10 Gyr. Also plotted as red lines are analytical normal fits … view at source ↗

Discussion (0). Continue with ORCID to comment.

Reference graph

Works this paper leans on

34 extracted references · 28 canonical work pages

  1. [1]

    G., Camisassa, M

    Althaus, L. G., Camisassa, M. E., Miller Bertolami, M. M., Có rsico, A. H., & García-Berro, E. 2015, A&A, 576, A9

    work page 2015

  2. [2]

    G., Córsico, A

    Althaus, L. G., Córsico, A. H., Isern, J., & García-Berro, E. 2010, A&A Rev., 18, 471

    2010

  3. [3]

    2017, MNRAS, 469, 2102

    Anguiano, B., Rebassa-Mansergas, A., García-Berro, E., et al. 2017, MNRAS, 469, 2102

    work page 2017

  4. [4]

    2008, A& A, 490, 135

    Antoja, T., Figueras, F., Fernández, D., & Torra, J. 2008, A& A, 490, 135

    work page 2008

  5. [5]

    2010, Lecture Notes and Essays in Astrophysics, 4, 13

    Antoja, T., Figueras, F., Torra, J., V alenzuela, O., & Picha rdo, B. 2010, Lecture Notes and Essays in Astrophysics, 4, 13

    work page 2010

  6. [6]

    2012, MNRAS, 426, L1

    Antoja, T., Helmi, A., Bienayme, O., et al. 2012, MNRAS, 426, L1

    2012

  7. [7]

    S., Feltzing, S., & Gustafsson, B

    Bensby, T., Oey, M. S., Feltzing, S., & Gustafsson, B. 2007, A pJ, 655, L89

    work page 2007

  8. [8]

    Bobylev, V . V . & Bajkova, A. T. 2016, Astronomy Letters, 42, 90

    work page 2016

Show all 34 references
  1. [9]

    & Hogg, D

    Bovy, J. & Hogg, D. W. 2010, ApJ, 717, 617

    2010

  2. [10]

    E., Althaus, L

    Camisassa, M. E., Althaus, L. G., Córsico, A. H., et al. 2018, arXiv e-prints [arXiv:1807.03894]

    2018 arXiv

  3. [11]

    E., Althaus, L

    Camisassa, M. E., Althaus, L. G., Córsico, A. H., et al. 2016, ApJ, 823, 158 Cánovas, H., Cantero, C., Cieza, L., et al. 2019, arXiv e-pri nts [arXiv:1902.07600]

    2016 arXiv

  4. [12]

    1997, A&A, 318 , 29

    Chen, B., Asiain, R., Figueras, F., & Torra, J. 1997, A&A, 318 , 29

    1997

  5. [13]

    1998, AJ, 115, 2384

    Dehnen, W. 1998, AJ, 115, 2384

    1998

  6. [14]

    Eggen, O. J. 1958, MNRAS, 118, 154

    1958

  7. [15]

    2005, A&A, 430, 165

    Famaey, B., Jorissen, A., Luri, X., et al. 2005, A&A, 430, 165

    2005

  8. [16]

    2001, PASP , 113, 409

    Fontaine, G., Brassard, P ., & Bergeron, P . 2001, PASP , 113, 409

    2001

  9. [17]

    2019, MNRAS, 1815

    Fragkoudi, F., Katz, D., Trick, W., et al. 2019, MNRAS, 1815

    2019

  10. [18]

    & Dettbarn, C

    Fuchs, B. & Dettbarn, C. 2011, AJ, 141, 5

    2011

  11. [19]

    2001, A&A, 373, 511 Gaia Collaboration, Katz, D., Antoja, T., et al

    Fux, R. 2001, A&A, 373, 511 Gaia Collaboration, Katz, D., Antoja, T., et al. 2018a, A&A, 616, A11 Gaia Collaboration, Katz, D., Antoja, T., et al. 2018b, A&A, 616, A11 García-Berro, E. & Oswalt, T. D. 2016, New A Rev., 72, 1 Gentile Fusillo, N. P ., Tremblay, P .-E., Gänsicke,...

    2001

  12. [20]

    2019, MNRAS, 484, 4 540

    Hattori, K., Gouda, N., Tagawa, H., et al. 2019, MNRAS, 484, 4 540

    2019

  13. [21]

    Hunt, J. A. S. & Bovy, J. 2018, MNRAS, 477, 3945

    2018

  14. [22]

    Hunt, J. A. S., Bovy, J., Pérez-Villegas, A., et al. 2018, MNR AS, 474, 95 Jiménez-Esteban, F. M., Torres, S., Rebassa-Mansergas, A. , et al. 2018, MN- RAS, 480, 4505

    2018

  15. [23]

    2018, ApJ, 860, L1 1

    Koppelman, H., Helmi, A., & V eljanoski, J. 2018, ApJ, 860, L1 1

    2018

  16. [24]

    & Shen, J

    Li, Z.-Y . & Shen, J. 2019, arXiv e-prints, arXiv:1904.03314

    2019 arXiv

  17. [25]

    L., Zhao, J

    Liang, X. L., Zhao, J. K., Oswalt, T. D., et al. 2017, ApJ, 844, 152

    2017

  18. [26]

    2006, A&A, 447, 173 Pérez-Villegas, A., Portail, M., Wegg, C., & Gerhard, O

    Pauli, E.-M., Napiwotzki, R., Heber, U., Altmann, M., & Oden kirchen, M. 2006, A&A, 447, 173 Pérez-Villegas, A., Portail, M., Wegg, C., & Gerhard, O. 201 7, ApJ, 840, L2

    2006

  19. [27]

    2015, MNRAS, 448, 713

    Portail, M., Wegg, C., Gerhard, O., & Martinez-V alpuesta, I . 2015, MNRAS, 448, 713

    2015

  20. [28]

    2018, A&A, 619, A72

    Ramos, P ., Antoja, T., & Figueras, F. 2018, A&A, 619, A72

    2018

  21. [29]

    R., Girven, J., & Gänsicke, B

    Rebassa-Mansergas, A., Nebot Gómez-Morán, A., Schreiber, M. R., Girven, J., & Gänsicke, B. T. 2011, MNRAS, 413, 1121

    2011

  22. [30]

    Reid, I. N. 2005, ARA&A, 43, 247

    2005

  23. [31]

    2019, arXiv e-prints, arXiv:1906.08009

    Tononi, J., Torres, S., García-Berro, E., et al. 2019, arXiv e-prints, arXiv:1906.08009

    2019 arXiv

  24. [32]

    2019 , MNRAS, 485, 5573

    Torres, S., Cantero, C., Rebassa-Mansergas, A., et al. 2019 , MNRAS, 485, 5573

    2019

  25. [33]

    2001, MNRAS, 328, 492

    Torres, S., García-Berro, E., Burkert, A., & Isern, J. 2001, MNRAS, 328, 492

    2001

  26. [34]

    2015, MNRAS, 450, 4050 Article number, page 5 of 5

    Wegg, C., Gerhard, O., & Portail, M. 2015, MNRAS, 450, 4050 Article number, page 5 of 5

    2015

Pith tools

Reviewed August 14, 2026 · model on record in the stance chip above.