Pith. sign in

REVIEW 3 major objections 5 minor 184 references

Is the composition of the Solar atmosphere unusual, and if so, why? Possible interpretations

T0 review · 3 major / 5 minor · reviewed 2026-08-05 · deepseek-v4-flash

Pith's one-line read The Sun's atmosphere appears genuinely unusual in its volatile-to-refractory element mix, and the cause remains unresolved.

desk verdict A useful, honest review of the Meléndez effect that undercuts its own premise with the GCE/age-curvature alternative — the anomaly may be an artifact. read the letter →

arxiv 2509.03435 v1 pith:HRQBL6RG submitted 2025-09-03 astro-ph.SR astro-ph.EP

classification astro-ph.SRastro-ph.EP
keywords Sun:abundancesStars:solartwinsMeléndezeffectcondensationtemperatureprotoplanetarydisksplanetformationgalacticchemicalevolution
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

The paper seeks to establish that the Sun's photosphere is genuinely unusual among solar-type stars: it is richer in volatile elements (C, N, O, S, P, Zn) relative to refractory elements (Ba, Ca, Ti, Y, Al, Sc, Zr) by 10–20% compared with the average solar twin. The author reviews the evidence, finds the pattern survives scrutiny, and then assesses every proposed mechanism — galactic chemical evolution, dust–gas separation in clouds, protoplanetary-disk outflows and accretion, planet engulfment, and atomic diffusion. No single explanation is uniquely established; the paper concludes that several processes may act together. The stakes are that whichever mechanism is right, the effect is a fossil of Solar System formation and a potential diagnostic of planetary systems around other stars.

What carries the argument

The key object is the Meléndez effect (ME): the correlation between the differential abundance offset Δ[X/Fe] for the Sun relative to solar twins and each element's condensation temperature Tc. The roughly two-branch correlation shown for the original 11 twins has an amplitude near 0.08 dex and is the single observational target that every candidate mechanism must reproduce. The method that makes it measurable is strictly differential spectroscopy of solar twins against asteroid-reflected sunlight, which cancels most systematic modeling errors and leaves a claimed error floor near 0.01–0.02 dex.

What would settle it

A high-precision differential re-analysis of the Sun against a large sample of solar twins, using 3D NLTE models for all elements and matching stars in age and birth radius, that returns a volatile-refractory slope indistinguishable from zero would falsify the claim that the Meléndez effect is real.

Watch

Extended reading notes

Core claim

The central claim is that the Sun's photosphere is anomalously rich in volatile elements relative to refractory ones when compared with most solar twins: a systematic offset of up to about 0.08 dex (10–20%) that scales with each element's condensation temperature. This Meléndez effect has been confirmed in independent samples, with roughly 5–15% of solar-type stars showing a similar pattern. The review finds that no proposed mechanism — galactic chemical evolution, dust-clearing in clouds, disk outflows and accretion, giant-planet pressure bumps, rocky-planet engulfment, or atomic diffusion — is both necessary and sufficient. The author's stated conclusion is that no definitive answer exists

Load-bearing premise

The measured 10–20% volatile excess is a true difference in the Sun's photospheric composition rather than a residual systematic error of differential spectral analysis.

Editorial extensions

If this is right

  • The Sun's pattern is shared by only a minority (roughly 5–15%) of solar-type stars, so it records an unusual formation history if real.
  • If the effect stems from a giant planet trapping pebbles outside a disk gap, volatile-rich stars should statistically host distant gas giants, a prediction that can be tested with existing exoplanet surveys.
  • Planet engulfment in binary stars reproduces refractory-rich companions and yields some ME-like patterns, but faces mixing time-scale constraints that limit how long the signature lasts.
  • Rocky planets as refractory reservoirs may contribute, but likely not alone, because disk dispersal times and the deep early solar convection zone weaken the visible signature.
  • No current mechanism uniquely explains the effect; the review points to cluster studies, cloud simulations, and co-moving pairs as the productive next tests.

Reading between the lines

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

  • The predicted rate of ME-like stars (about 5–15% of solar-type stars) suggests a direct test: if Jupiter-style pebble-trapping is responsible, those stars should show a statistically significant excess of giant planets at a few AU, a measurement within reach of current surveys.
  • Co-moving and wide-binary pairs may be the cleanest discriminator: ME-like differences within coeval pairs would rule out galactic chemical evolution as the whole story and point to local disk or accretion processes.
  • Repeating the differential analysis with 3D-NLTE predictions for every element, rather than just a handful, could reveal whether the residual 0.02-dex error floor hides an element-by-element pattern that identifies specific dust species or condensation sequences.
  • The habitability link is suggestive at most: the paper itself notes any connection is probably indirect, mediated by the same Jupiter–Saturn orbital architecture that may produce the ME.
Share X Bluesky LinkedIn Reddit HN

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 5 minor

Summary. This review article assesses the evidence for and possible causes of the 'Meléndez effect' (ME): the claim that the solar photosphere is enhanced by 10–20% in volatile elements (C, N, O, S, P, Zn) relative to refractory elements (Ba, Ca, Ti, Y, Al, Sc, Zr) compared with most solar twins. The paper first discusses absolute and differential abundance determinations, then systematically reviews candidate explanations: galactic chemical evolution and solar migration, a local supernova, dust-cleansing and gas–dust separation in star-forming regions, protoplanetary disk fractionation and outflows, planet formation and engulfment, abundance differences in stellar pairs, atomic diffusion and mixing, and possible links to habitability. It concludes that no definitive explanation exists and that several mechanisms may contribute jointly.

Significance. If the Meléndez effect is real, it is an important boundary condition for Solar System formation and a potential tracer of planetary processes. The manuscript is valuable as a broad, up-to-date critical review: it covers independent work by several groups, includes quantitative time-scale and yield arguments (e.g., thermohaline mixing in §6, self-cleansing accretion limits in §4.3, supernova yield matching in §3.2), and identifies falsifiable tests (e.g., the Teff dependence of binary abundance differences, §6; M67 abundance patterns, §3.3). The review is also honest in admitting where models fail or remain speculative. However, the paper's central premise—that the ME is a genuine compositional anomaly—is never securely established against the strongest available counterargument (Cowley & Yüce 2022), and this undermines the framing of all subsequent sections.

major comments (3)
  1. [Sections 2.3 and 3.1] The paper's central premise is left in a contradictory state. Cowley & Yüce (2022) found that quadratic abundance–age relations for the Bedell et al. (2018) sample make the Sun non-anomalous among solar-age twins. The author dismisses this result only by saying it is 'affected by inclusion of stars with ages above 6.0 Gyrs' (§3.1), without providing a quantitative re-analysis or showing how the conclusion changes when those stars are removed. In the very next paragraph, the author's own Fig. 6 shows that the quadratic coefficients b correlate with condensation temperature and states that this 'would seem to explain the ME as an effect of the galactic chemical evolution.' That is precisely the GCE alternative that would dissolve the ME. Yet §2.3 states that 'it will be assumed that the ME reflects some processes' and §§4–7 discuss only Solar-System mechanisms. The manuscript needs either
  2. [Section 3.1, Fig. 6] The b–Tc regression that supports the GCE interpretation is computed after removing C, O, and Ba as 'outliers' (red crosses), without stating an outlier criterion or performing a sensitivity analysis. C and O are among the principal volatile elements that define the ME; excluding them is not neutral. The correlation may be an artifact of this selection. The author should report fits with and without all three points, quantify the influence of each excluded element, and justify the exclusions on grounds independent of the hypothesis being tested.
  3. [Section 2.2] The estimated differential error floor of ~0.02 dex (0.01 dex for some elements) is based on a limited set of elements: O, C, Fe, and Mn. This estimate is then extrapolated to all elements contributing to the ME, including S, P, and Zn, for which 3D-NLTE differential corrections are largely missing. Given that the ME amplitude is ~0.08 dex, a 0.02–0.03 dex floor is tolerable, but the paper should explicitly acknowledge that an error floor of ~0.04 dex for untested elements would make the ME non-significant for some elements. The current text moves too quickly from 'reasonable to assume' to 'it will be assumed that the ME reflects some processes.'
minor comments (5)
  1. [Section 3.1, Fig. 6] The figure would benefit from error bars on the b coefficients and from a clear statement of the fitted slope, intercept, and scatter. The text also says 'A fitted line to the rest of the points' but does not identify which points (beyond the three red crosses) are included or whether the fit is weighted.
  2. [Section 5.2] In the sentence beginning 'The authors modelled the resulting abundance effects...', the antecedent is unclear; it should be 'Hühn and Bitsch (2023) modelled...' for readability.
  3. [Section 8] 'as long as the PH value is kept' should be 'pH value'.
  4. [Section 2.3] Typographical spacing in 'Meléndez effect(ME )' and 'the Meléndez effect(ME )' appears inconsistent; unify.
  5. [Section 3.1] The phrase 'for a test' in 'This hypothesis can be tested by plotting...' is slightly awkward; consider rewording to 'This hypothesis can be tested directly by plotting...'.

Circularity Check

0 steps flagged · score 0.0 of 10

No circularity: a self-aware review of a contested observational effect; self-citations are supported by independent studies and the author explicitly declines to derive a forced explanation.

full rationale

This is a review, not a derivation. The Meléndez effect is an empirical differential-abundance pattern first reported in Meléndez et al. (2009), on which Gustafsson is a co-author, but §2.3 explicitly lists independent confirmations: Ramírez et al. (2010, 2014), Adibekyan et al. (2014), Nissen (2015, 2016), Bedell et al. (2018), Rampalli et al. (2024). The central premise is therefore not supported only by self-citation. The paper's own dust-cleansing models (Gustafsson 2018a,b) are cited as possible mechanisms and are ultimately assessed as 'not a very probable explanation' in §9; they are not load-bearing predictions. The working assumption in §2.3 — 'In the following it will be assumed that the ME reflects some processes in the Galaxy, in the early evolution of the solar nebula or the solar system' — is explicitly an assumption, not a derived conclusion; the paper repeatedly states that no definitive answer has been found (§9). The Cowley & Yüce (2022) quadratic age-fit alternative that would dissolve the ME is quoted and discussed in §3.1: the author notes it 'would seem to explain the ME as an effect of the galactic chemical evolution' but leaves it unresolved. That is an acknowledged internal tension/correctness risk, not a circular reduction: the review does not define the ME in terms of the explanations or fit a parameter and then rename it a prediction. The Nordlund (2025) disk-outflow model has a free parameter r whose value sets the curvature (Fig. 9), but the figure is presented as model outcomes for different r with an explicitly normalized amplitude, and the paper does not claim an independent prediction from it. No equation or fitted quantity is shown to be identical by construction to the phenomenon it is said to explain. Hence no significant circularity.

Assumptions & free parameters 2 free parameters · 3 assumptions · 0 invented entities

The paper itself introduces no new physical entities and no new free parameters beyond two illustrative fits (Fig. 6 regression and Fig. 9 normalization). Its conclusions rest mainly on the assumed reality of the Melendez effect and on standard time-scale or condensation-temperature assumptions inherited from the literature.

free parameters (2)
  • Linear regression slope and intercept of quadratic-coefficient vs Tc (Fig. 6) = not quoted numerically in text
    These coefficients are fit to the bb values from Cowley and Yuce (2022) after excluding C, O, and Ba; the resulting correlation is used to raise the possibility that the ME is a galactic evolution artifact.
  • Normalization amplitude for the Nordlund (2025) outflow-model curve in Fig. 9 = chosen to match the observed amplitude
    The theoretical delta-e amplitude is rescaled to match the observed ME amplitude, so the match shown does not test the model's predicted amplitude.
assumptions (3)
  • domain assumption Differential abundance errors in solar twin comparisons are reduced to about 0.02 dex (0.01 dex in some cases) for most elements.
    The review assumes the ME is not dominated by residual systematic errors (Section 2.2), and later 'it will be assumed that the ME reflects some processes' (Section 2.3).
  • domain assumption The condensation temperature scale of Lodders (2003) provides a meaningful ordering of elements for the fractionation processes considered.
    Used throughout, e.g., Fig. 1 and all scenario discussions, as the independent variable for the ME.
  • domain assumption Published Galactic chemical evolution corrections (e.g., Bedell et al. linear fits, Cowley and Yuce quadratic fits) are valid representations of abundance-age relations.
    Sections 3.1 and 3.2 discuss the viability of these corrections; the curvature hypothesis in Fig. 6 depends on this assumption.

how reviews work

0 comments
Cite this review

Pith. "Pith review of Is the composition of the Solar atmosphere unusual, and if so, why? Possible interpretations." pith.science (2026). https://pith.science/paper/HRQBL6RG

@misc{pith2026250903435,
  author       = {Pith},
  title        = {Pith review of: Is the composition of the Solar atmosphere unusual, and if so, why? Possible interpretations},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/HRQBL6RG}},
  note         = {Machine review of arXiv:2509.03435}
}
read the original abstract

The ongoing discussion about the atomic chemical composition of the Sun is commented on. The main focus in this review is on the deviation of the solar composition from that of most other solar-type stars in that its ratio of volatiles (like the elements C, N, O, S, P and Zn) to the refractories (most metals, like Ba, Ca, Ti, Y, Al, Sc and Zr) tends to be higher in the Sun by 10 to 20%. What does this tell about the formation and evolution of the Solar System? Scenarios in terms of galactic evolution, formation of the pre-solar nebula, of the evolution of the protoplanetary disk, of the engulfing of planets, and of other processes within the Solar System are considered, as well as the evolution of binary stars with similarly different chemical composition. Finally, implications, if any, on the habitability of the Solar System are commented on.

Discussion (0). Sign in to comment.

Reference graph

Works this paper leans on

184 extracted references · 47 canonical work pages

  1. [1]

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

    ENTRY address archive author booktitle chapter doi edition editor eid eprint howpublished institution journal key keywords month note number organization pages publisher school series title type url volume year archivePrefix primaryClass adsurl adsnote version label extra.label sort.label short.list INTEGERS output.state before.all mid.sentence after.sent...

  2. [2]

    write newline

    " write newline "" before.all 'output.state := FUNCTION add.period duplicate empty 'skip "." * add.blank if FUNCTION if.digit duplicate "0" = swap duplicate "1" = swap duplicate "2" = swap duplicate "3" = swap duplicate "4" = swap duplicate "5" = swap duplicate "6" = swap duplicate "7" = swap duplicate "8" = swap "9" = or or or or or or or or or FUNCTION ...

  3. [3]

    In: Bulletin of the American Astronomical Society, p 268

    Abt HA, Levy SG (1975) The Binary Frequency Among Solar-Type Stars. In: Bulletin of the American Astronomical Society, p 268

  4. [4]

    T _ c trends and clues to Galactic evolution

    Adibekyan VZ, Gonz \'a lez Hern \'a ndez JI, Delgado Mena E, et al (2014) On the origin of stars with and without planets. T _ c trends and clues to Galactic evolution . 564:L15. doi:10.1051/0004-6361/201423435, https://arxiv.org/abs/1404.4514 https://arxiv.org/abs/arXiv:1404.4514 [astro-ph.SR]

  5. [5]

    In: Beuther H, Klessen RS, Dullemond CP, et al (eds) Protostars and Planets VI, pp 475--496, doi:10.2458/azu_uapress_9780816531240-ch021, 1311.1819

    Alexander R, Pascucci I, Andrews S, et al (2014) The Dispersal of Protoplanetary Disks . In: Beuther H, Klessen RS, Dullemond CP, et al (eds) Protostars and Planets VI, pp 475--496, doi:10.2458/azu_uapress_9780816531240-ch021, 1311.1819

  6. [6]

    Implications of 3D non-LTE spectral line formation

    Amarsi AM, Nissen PE, Sk \'u lad \'o ttir \'A (2019) Carbon, oxygen, and iron abundances in disk and halo stars. Implications of 3D non-LTE spectral line formation . 630:A104. doi:10.1051/0004-6361/201936265, https://arxiv.org/abs/1908.10319 https://arxiv.org/abs/arXiv:1908.10319 [astro-ph.SR]

  7. [7]

    656:A113

    Amarsi AM, Grevesse N, Asplund M, et al (2021) The solar carbon, nitrogen, and oxygen abundances from a 3D LTE analysis of molecular lines . 656:A113. doi:10.1051/0004-6361/202141384, https://arxiv.org/abs/2109.04752 https://arxiv.org/abs/arXiv:2109.04752 [astro-ph.SR]

  8. [8]

    Amarsi AM, Liljegren S, Nissen PE (2022) 3D non-LTE iron abundances in FG-type dwarfs . 668:A68. doi:10.1051/0004-6361/202244542, https://arxiv.org/abs/2209.13449 https://arxiv.org/abs/arXiv:2209.13449 [astro-ph.SR]

Show all 184 references
  1. [9]

    43(1):481--530

    Asplund M (2005) New Light on Stellar Abundance Analyses: Departures from LTE and Homogeneity . 43(1):481--530. doi:10.1146/annurev.astro.42.053102.134001

  2. [10]

    In: Barnes TGIII, Bash FN (eds) Cosmic Abundances as Records of Stellar Evolution and Nucleosynthesis, p 25

    Asplund M, Grevesse N, Sauval AJ (2005) The Solar Chemical Composition . In: Barnes TGIII, Bash FN (eds) Cosmic Abundances as Records of Stellar Evolution and Nucleosynthesis, p 25

  3. [11]

    47(1):481--522

    Asplund M, Grevesse N, Sauval AJ, et al (2009) The Chemical Composition of the Sun . 47(1):481--522. doi:10.1146/annurev.astro.46.060407.145222, https://arxiv.org/abs/0909.0948 https://arxiv.org/abs/arXiv:0909.0948 [astro-ph.SR]

  4. [12]

    653:A141

    Asplund M, Amarsi AM, Grevesse N (2021) The chemical make-up of the Sun: A 2020 vision . 653:A141. doi:10.1051/0004-6361/202140445, https://arxiv.org/abs/2105.01661 https://arxiv.org/abs/arXiv:2105.01661 [astro-ph.SR]

  5. [13]

    HC (2012) RNA Folding and Catalysis Mediated by Iron (II)

    Athavale SS, Petrov AS, et al. HC (2012) RNA Folding and Catalysis Mediated by Iron (II) . PLOS ONE 7(5):1--7. doi:10.1371/journal.pone.0038024

  6. [14]

    526(4):6088--6102

    Baba J, Saitoh TR, Tsujimoto T (2023) Exploring the Sun's birth radius and the distribution of planet building blocks in the Milky Way galaxy: a multizone Galactic chemical evolution approach . 526(4):6088--6102. doi:10.1093/mnras/stad3188, https://arxiv.org/abs/2310.10335 htt...

  7. [15]

    In: Inutsuka S, Aikawa Y, Muto T, et al (eds) Protostars and Planets VII, p 423, doi:10.48550/arXiv.2210.13314, 2210.13314

    Bae J, Isella A, Zhu Z, et al (2023) Structured Distributions of Gas and Solids in Protoplanetary Disks . In: Inutsuka S, Aikawa Y, Muto T, et al (eds) Protostars and Planets VII, p 423, doi:10.48550/arXiv.2210.13314, 2210.13314

  8. [16]

    Nature Communications 7:13639

    Banerjee P, Qian YZ, Heger A, et al (2016) Evidence from stable isotopes and ^ 10 Be for solar system formation triggered by a low-mass supernova . Nature Communications 7:13639. doi:10.1038/ncomms13639, https://arxiv.org/abs/1611.07162 https://arxiv.org/abs/arXiv:1611.07162 [...

  9. [17]

    Baraffe I, Chabrier G (2010) Effect of episodic accretion on the structure and the lithium depletion of low-mass stars and planet-hosting stars . 521:A44. doi:10.1051/0004-6361/201014979, https://arxiv.org/abs/1008.4288 https://arxiv.org/abs/arXiv:1008.4288 [astro-ph.EP]

  10. [18]

    Barklem PS (2016) Accurate abundance analysis of late-type stars: advances in atomic physics . 24(1):9. doi:10.1007/s00159-016-0095-9, https://arxiv.org/abs/1604.07659 https://arxiv.org/abs/arXiv:1604.07659 [astro-ph.SR]

  11. [19]

    514(2):2145--2161

    Bate MR (2022) Dust coagulation during the early stages of star formation: molecular cloud collapse and first hydrostatic core evolution . 514(2):2145--2161. doi:10.1093/mnras/stac1391, https://arxiv.org/abs/2205.07681 https://arxiv.org/abs/arXiv:2205.07681 [astro-ph.GA]

  12. [20]

    Baumann P, Ram \' rez I, Mel \'e ndez J, et al (2010) Lithium depletion in solar-like stars: no planet connection . 519:A87. doi:10.1051/0004-6361/201015137, https://arxiv.org/abs/1008.0575 https://arxiv.org/abs/arXiv:1008.0575 [astro-ph.SR]

  13. [21]

    865(1):68

    Bedell M, Bean JL, Mel \'e ndez J, et al (2018) The Chemical Homogeneity of Sun-like Stars in the Solar Neighborhood . 865(1):68. doi:10.3847/1538-4357/aad908, https://arxiv.org/abs/1802.02576 https://arxiv.org/abs/arXiv:1802.02576 [astro-ph.SR]

  14. [22]

    521(2):2969--2987

    Behmard A, Dai F, Brewer JM, et al (2023) Planet engulfment detections are rare according to observations and stellar modelling . 521(2):2969--2987. doi:10.1093/mnras/stad745, https://arxiv.org/abs/2210.12121 https://arxiv.org/abs/arXiv:2210.12121 [astro-ph.EP]

  15. [23]

    In: Niemczura E, Smalley B, Pych W (eds) Determination of Atmospheric Parameters of B

    Bergemann M, Serenelli A (2014) Solar Abundance Problem . In: Niemczura E, Smalley B, Pych W (eds) Determination of Atmospheric Parameters of B. p 245--258, doi:10.1007/978-3-319-06956-2_21

  16. [24]

    Bergemann M, Gallagher AJ, Eitner P, et al (2019) Observational constraints on the origin of the elements. I. 3D NLTE formation of Mn lines in late-type stars . 631:A80. doi:10.1051/0004-6361/201935811, https://arxiv.org/abs/1905.05200 https://arxiv.org/abs/arXiv:1905.05200 [a...

  17. [25]

    508(2):2236--2253

    Bergemann M, Hoppe R, Semenova E, et al (2021) Solar oxygen abundance . 508(2):2236--2253. doi:10.1093/mnras/stab2160, https://arxiv.org/abs/2109.01143 https://arxiv.org/abs/arXiv:2109.01143 [astro-ph.SR]

  18. [26]

    arXiv e-prints arXiv:2503.05402

    Bergemann M, Lodders K, Palme H (2025) The Chemical Composition of the Sun . arXiv e-prints arXiv:2503.05402. doi:10.48550/arXiv.2503.05402, https://arxiv.org/abs/2503.05402 https://arxiv.org/abs/arXiv:2503.05402 [astro-ph.SR]

  19. [27]

    855(2):115

    Berger TA, Howard AW, Boesgaard AM (2018) Identifying Young Kepler Planet Host Stars from Keck-HIRES Spectra of Lithium . 855(2):115. doi:10.3847/1538-4357/aab154, https://arxiv.org/abs/1802.09529 https://arxiv.org/abs/arXiv:1802.09529 [astro-ph.EP]

  20. [28]

    doi:10.1093/mnras/sty1011, https://arxiv.org/abs/1804.06293 https://arxiv.org/abs/arXiv:1804.06293 [astro-ph.SR]

    Bertelli Motta C, Pasquali A, Richer J, et al (2018) The Gaia-ESO Survey: evidence of atomic diffusion in M67? 478(1):425--438. doi:10.1093/mnras/sty1011, https://arxiv.org/abs/1804.06293 https://arxiv.org/abs/arXiv:1804.06293 [astro-ph.SR]

  21. [29]

    Biazzo K, Gratton R, Desidera S, et al (2015) The GAPS programme with HARPS-N at TNG. X. Differential abundances in the XO-2 planet-hosting binary . 583:A135. doi:10.1051/0004-6361/201526375, https://arxiv.org/abs/1506.01614 https://arxiv.org/abs/arXiv:1506.01614 [astro-ph.SR]

  22. [30]

    493(4):5079--5088

    Booth RA, Owen JE (2020) Fingerprints of giant planets in the composition of solar twins . 493(4):5079--5088. doi:10.1093/mnras/staa578, https://arxiv.org/abs/2002.11135 https://arxiv.org/abs/arXiv:2002.11135 [astro-ph.EP]

  23. [31]

    Brucalassi A, Koppenhoefer J, Saglia R, et al (2017) Search for giant planets in M 67. IV. Survey results . 603:A85. doi:10.1051/0004-6361/201527562, https://arxiv.org/abs/1703.04296 https://arxiv.org/abs/arXiv:1703.04296 [astro-ph.EP]

  24. [32]

    686:A108

    Buldgen G, Noels A, Scuflaire R, et al (2024) In-depth analysis of solar models with high-metallicity abundances and updated opacity tables . 686:A108. doi:10.1051/0004-6361/202348312, https://arxiv.org/abs/2404.10478 https://arxiv.org/abs/arXiv:2404.10478 [astro-ph.SR]

  25. [33]

    Caffau E, Ludwig HG, Steffen M, et al (2008) The photospheric solar oxygen project. I. Abundance analysis of atomic lines and influence of atmospheric models . 488(3):1031--1046. doi:10.1051/0004-6361:200809885, https://arxiv.org/abs/0805.4398 https://arxiv.org/abs/arXiv:0805....

  26. [34]

    Solar Physics 268(2):255--269

    Caffau E, Ludwig HG, Steffen M, et al (2011) Solar Chemical Abundances Determined with a CO5BOLD 3D Model Atmosphere . Solar Physics 268(2):255--269. doi:10.1007/s11207-010-9541-4, https://arxiv.org/abs/1003.1190 https://arxiv.org/abs/arXiv:1003.1190 [astro-ph.SR]

  27. [35]

    Caffau E, Ludwig HG, Steffen M, et al (2015) The photospheric solar oxygen project. III. Investigation of the centre-to-limb variation of the 630 nm [O I]-Ni I blend . 579:A88. doi:10.1051/0004-6361/201526331, https://arxiv.org/abs/1506.00931 https://arxiv.org/abs/arXiv:1506.0...

  28. [36]

    Problems of Cosmogeny 7:91

    Cameron AGW (1964) Remarks on the Formation of the Solar System from the Point of View of Nucleogenesis . Problems of Cosmogeny 7:91

  29. [37]

    15(1):121--146

    Cameron AGW (1973) Abundances of the Elements in the Solar System . 15(1):121--146. doi:10.1007/BF00172440

  30. [38]

    arXiv e-prints arXiv:2505.22615

    Carlos M, Amarsi AM, Nissen PE, et al (2025) The peculiar composition of the Sun is not related to giant planets . arXiv e-prints arXiv:2505.22615. https://arxiv.org/abs/2505.22615 https://arxiv.org/abs/arXiv:2505.22615 [astro-ph.SR]

  31. [39]

    Carlsson M, Hansteen VH, Gudiksen BV, et al (2016) A publicly available simulation of an enhanced network region of the Sun . 585:A4. doi:10.1051/0004-6361/201527226, https://arxiv.org/abs/1510.07581 https://arxiv.org/abs/arXiv:1510.07581 [astro-ph.SR]

  32. [40]

    94:1--11

    Cayrel de Strobel G, Knowles N, Hernandez G, et al (1981) In search of real solar twins. 94:1--11

  33. [41]

    724(1):92--97

    Chambers JE (2010) Stellar Elemental Abundance Patterns: Implications for Planet Formation . 724(1):92--97. doi:10.1088/0004-637X/724/1/92

  34. [42]

    Living Reviews in Solar Physics 18(1):2

    Christensen-Dalsgaard J (2021) Solar structure and evolution . Living Reviews in Solar Physics 18(1):2. doi:10.1007/s41116-020-00028-3, https://arxiv.org/abs/2007.06488 https://arxiv.org/abs/arXiv:2007.06488 [astro-ph.SR]

  35. [43]

    121(877):213

    Churchwell E, Babler BL, Meade MR, et al (2009) The Spitzer/GLIMPSE Surveys: A New View of the Milky Way . 121(877):213. doi:10.1086/597811

  36. [44]

    Codella C, Podio L, Garufi A, et al (2020) ALMA chemical survey of disk-outflow sources in Taurus (ALMA-DOT). IV. Thioformaldehyde (H _ 2 CS) in protoplanetary discs: spatial distributions and binding energies . 644:A120. doi:10.1051/0004-6361/202039309, https://arxiv.org/abs/...

  37. [45]

    512(3):3684--3690

    Cowley CR, Y \"u ce K (2022) Galactic chemical evolution of the solar neighbourhood, solar twins, and exoplanet indicators . 512(3):3684--3690. doi:10.1093/mnras/stac637, https://arxiv.org/abs/2203.05592 https://arxiv.org/abs/arXiv:2203.05592 [astro-ph.SR]

  38. [46]

    Delbouille L, Roland G, Neven L (1973) Atlas photometrique du spectre solaire de [lambda] 3000 a [lambda] 10000

  39. [47]

    Extending the sample

    Delgado Mena E, Israelian G, Gonz \'a lez Hern \'a ndez JI, et al (2014) Li depletion in solar analogues with exoplanets. Extending the sample . 562:A92. doi:10.1051/0004-6361/201321493, https://arxiv.org/abs/1311.6414 https://arxiv.org/abs/arXiv:1311.6414 [astro-ph.EP]

  40. [48]

    Delgado Mena E, Bertr \'a n de Lis S, Adibekyan VZ, et al (2015) Li abundances in F stars: planets, rotation, and Galactic evolution . 576:A69. doi:10.1051/0004-6361/201425433, https://arxiv.org/abs/1412.4618 https://arxiv.org/abs/arXiv:1412.4618 [astro-ph.SR]

  41. [49]

    Investigating line broadening, magnetic fields, and model effects

    Deshmukh SA, Ludwig HG, Ku c inskas A, et al (2022) The solar photospheric silicon abundance according to CO ^ 5 BOLD. Investigating line broadening, magnetic fields, and model effects . 668:A48. doi:10.1051/0004-6361/202142072, https://arxiv.org/abs/2212.07485 https://arxiv.o...

  42. [50]

    840(2):99

    Dotter A, Conroy C, Cargile P, et al (2017) The Influence of Atomic Diffusion on Stellar Ages and Chemical Tagging . 840(2):99. doi:10.3847/1538-4357/aa6d10, https://arxiv.org/abs/1704.03465 https://arxiv.org/abs/arXiv:1704.03465 [astro-ph.SR]

  43. [51]

    663(2):866--894

    Draine BT, Dale DA, Bendo G, et al (2007) Dust Masses, PAH Abundances, and Starlight Intensities in the SINGS Galaxy Sample . 663(2):866--894. doi:10.1086/518306, https://arxiv.org/abs/astro-ph/0703213 https://arxiv.org/abs/arXiv:astro-ph/0703213 [astro-ph]

  44. [52]

    51(1):269--310

    Duch \^e ne G, Kraus A (2013) Stellar Multiplicity . 51(1):269--310. doi:10.1146/annurev-astro-081710-102602, https://arxiv.org/abs/1303.3028 https://arxiv.org/abs/arXiv:1303.3028 [astro-ph.SR]

  45. [53]

    p 39--43, doi:10.1007/3-540-54752-5_186

    Duquennoy A, Mayor M (1991) How Many Single Stars Among Solar Type Stars? In: Heidmann J, Klein MJ (eds) Bioastronomy: The Search for Extraterrestial Life The Exploration Broadens, vol 390. p 39--43, doi:10.1007/3-540-54752-5_186

  46. [54]

    Towards a consistent reference metallicity

    Fabbian D, Moreno-Insertis F, Khomenko E, et al (2012) Solar Fe abundance and magnetic fields. Towards a consistent reference metallicity . 548:A35. doi:10.1051/0004-6361/201219335, https://arxiv.org/abs/1209.2771 https://arxiv.org/abs/arXiv:1209.2771 [astro-ph.SR]

  47. [55]

    874(1):81

    Fernandes RB, Mulders GD, Pascucci I, et al (2019) Hints for a Turnover at the Snow Line in the Giant Planet Occurrence Rate . 874(1):81. doi:10.3847/1538-4357/ab0300, https://arxiv.org/abs/1812.05569 https://arxiv.org/abs/arXiv:1812.05569 [astro-ph.SR]

  48. [56]

    In: Gomes N, Ascenso J (eds) 24th Portuguese National Astronomy and Astrophysics Meeting, p 51

    Figueira P (2014) Lithium depletion of planetary-host stars . In: Gomes N, Ascenso J (eds) 24th Portuguese National Astronomy and Astrophysics Meeting, p 51

  49. [57]

    Astronomische Nachrichten 323:213--219

    Freytag B, Steffen M, Dorch B (2002) Spots on the surface of Betelgeuse -- Results from new 3D stellar convection models . Astronomische Nachrichten 323:213--219. doi:10.1002/1521-3994(200208)323:3/4<213::AID-ASNA213>3.0.CO;2-H

  50. [58]

    922(2):129

    Galarza JY, L \'o pez-Valdivia R, Mel \'e ndez J, et al (2021) Evidence of Rocky Planet Engulfment in the Wide Binary System HIP 71726/HIP 71737 . 922(2):129. doi:10.3847/1538-4357/ac2362

  51. [59]

    Cell 168(6)

    Goldford JE, Hartman H, Smith TF, et al (2017) Remnants of an Ancient Metabolism without Phosphate . Cell 168(6)

  52. [60]

    285(2):403--412

    Gonzalez G (1997) The stellar metallicity-giant planet connection . 285(2):403--412. doi:10.1093/mnras/285.2.403

  53. [61]

    118(849):1494--1505

    Gonzalez G (2006) The Chemical Compositions of Stars with Planets: A Review . 118(849):1494--1505. doi:10.1086/509792, https://arxiv.org/abs/astro-ph/0609829 https://arxiv.org/abs/arXiv:astro-ph/0609829 [astro-ph]

  54. [62]

    443:L99--L103

    Gonzalez G (2014) Solar system chemical abundances corrected for systematics. 443:L99--L103. doi:10.1093/mnrasl/slu083, https://arxiv.org/abs/1406.0480 https://arxiv.org/abs/arXiv:1406.0480 [astro-ph.SR]

  55. [63]

    In: Holt SS, Sonneborn G (eds) Cosmic Abundances, p 117

    Grevesse N, Noels A, Sauval AJ (1996) Standard Abundances . In: Holt SS, Sonneborn G (eds) Cosmic Abundances, p 117

  56. [64]

    doi:10.1023/A:1005164331058

    Gustafsson B (1998) Is the Sun a Sun-Like Star? 85:419--428. doi:10.1023/A:1005164331058

  57. [65]

    Gustafsson B (2018 a ) Dust cleansing of star-forming gas. I. Has radiation from bright stars affected the chemical composition of the Sun and M 67? 616:A91. doi:10.1051/0004-6361/201732354, https://arxiv.org/abs/1805.00547 https://arxiv.org/abs/arXiv:1805.00547 [astro-ph.GA]

  58. [66]

    Gustafsson B (2018 b ) Dust cleansing of star-forming gas. II. Did late accretion flows change the chemical composition of the solar atmosphere? 620:A53. doi:10.1051/0004-6361/201833353, https://arxiv.org/abs/1809.02361 https://arxiv.org/abs/arXiv:1809.02361 [astro-ph.SR]

  59. [67]

    328(1-2):185--191

    Gustafsson B, Mel \'e ndez J, Asplund M, et al (2010) The chemical composition of solar-type stars in comparison with that of the Sun . 328(1-2):185--191. doi:10.1007/s10509-009-0257-6

  60. [68]

    Condensation of Dust Particles

    Hasegawa H, Kozasa T (1988) Chapter 9. Condensation of Dust Particles . Progress of Theoretical Physics Supplement 96:107--120. doi:10.1143/PTPS.96.107

  61. [69]

    381:959--970

    Heiter U (2002) The abundance pattern of lambda Bootis stars . 381:959--970. doi:10.1051/0004-6361:20011593, https://arxiv.org/abs/astro-ph/0112196 https://arxiv.org/abs/arXiv:astro-ph/0112196 [astro-ph]

  62. [70]

    381:971--981

    Heiter U, Weiss WW, Paunzen E (2002) The accretion/diffusion theory for lambda Bootis stars in the light of spectroscopic data . 381:971--981. doi:10.1051/0004-6361:20011594, https://arxiv.org/abs/astro-ph/0112198 https://arxiv.org/abs/arXiv:astro-ph/0112198 [astro-ph]

  63. [71]

    526(1):534--547

    Higgins ER, Vink JS, Hirschi R, et al (2023) Stellar wind yields of very massive stars . 526(1):534--547. doi:10.1093/mnras/stad2537, https://arxiv.org/abs/2308.10941 https://arxiv.org/abs/arXiv:2308.10941 [astro-ph.SR]

  64. [72]

    In: Dworetsky MM, Castelli F, Faraggiana R (eds) IAU Colloq

    Holweger H, Sturenburg S (1993) Carbon and Silicon in Normal A-Stars and in Lambda-Bootis Stars . In: Dworetsky MM, Castelli F, Faraggiana R (eds) IAU Colloq. 138: Peculiar versus Normal Phenomena in A-type and Related Stars, p 356

  65. [73]

    456(4):4174--4190

    Hopkins PF, Lee H (2016) The fundamentally different dynamics of dust and gas in molecular clouds . 456(4):4174--4190. doi:10.1093/mnras/stv2745, https://arxiv.org/abs/1510.02477 https://arxiv.org/abs/arXiv:1510.02477 [astro-ph.GA]

  66. [74]

    Earth and Planetary Science Letters 487:9--20

    Huguet L, Van Orman JA, Hauck SA, et al (2018) Earth's inner core nucleation paradox . Earth and Planetary Science Letters 487:9--20. doi:10.1016/j.epsl.2018.01.018

  67. [75]

    H \"u hn LA, Bitsch B (2023) How accretion of planet-forming disks influences stellar abundances . 676:A87. doi:10.1051/0004-6361/202346604, https://arxiv.org/abs/2306.16461 https://arxiv.org/abs/arXiv:2306.16461 [astro-ph.EP]

  68. [76]

    363(1):293--314

    Hurley JR, Pols OR, Aarseth SJ, et al (2005) A complete N-body model of the old open cluster M67 . 363(1):293--314. doi:10.1111/j.1365-2966.2005.09448.x, https://arxiv.org/abs/astro-ph/0507239 https://arxiv.org/abs/arXiv:astro-ph/0507239 [astro-ph]

  69. [77]

    462(7270):189--191

    Israelian G, Delgado Mena E, Santos NC, et al (2009) Enhanced lithium depletion in Sun-like stars with orbiting planets . 462(7270):189--191. doi:10.1038/nature08483, https://arxiv.org/abs/0911.4198 https://arxiv.org/abs/arXiv:0911.4198 [astro-ph.SR]

  70. [78]

    800(2):L22

    Izidoro A, Raymond SN, Morbidelli A, et al (2015) Gas Giant Planets as Dynamical Barriers to Inward-Migrating Super-Earths . 800(2):L22. doi:10.1088/2041-8205/800/2/L22, https://arxiv.org/abs/1501.06308 https://arxiv.org/abs/arXiv:1501.06308 [astro-ph.EP]

  71. [79]

    470(2):1750--1770

    Izidoro A, Ogihara M, Raymond SN, et al (2017) Breaking the chains: hot super-Earth systems from migration and disruption of compact resonant chains . 470(2):1750--1770. doi:10.1093/mnras/stx1232, https://arxiv.org/abs/1703.03634 https://arxiv.org/abs/arXiv:1703.03634 [astro-ph.EP]

  72. [80]

    Jofr \'e P, Heiter U, Soubiran C, et al (2015) Gaia FGK benchmark stars: abundances of and iron-peak elements . 582:A81. doi:10.1051/0004-6361/201526604, https://arxiv.org/abs/1507.00027 https://arxiv.org/abs/arXiv:1507.00027 [astro-ph.SR]

  73. [81]

    57:571--616

    Jofr \'e P, Heiter U, Soubiran C (2019) Accuracy and Precision of Industrial Stellar Abundances . 57:571--616. doi:10.1146/annurev-astro-091918-104509, https://arxiv.org/abs/1811.08041 https://arxiv.org/abs/arXiv:1811.08041 [astro-ph.SR]

  74. [82]

    In: American Astronomical Society Meeting Abstracts, p 340.04D

    Johnson J (2023) The Milky Way as a Case Study of Galactic Chemical Evolution . In: American Astronomical Society Meeting Abstracts, p 340.04D

  75. [83]

    863(2):191

    Jones T, Stark DP, Ellis RS (2018) Dust in the Wind: Composition and Kinematics of Galaxy Outflows at the Peak Epoch of Star Formation . 863(2):191. doi:10.3847/1538-4357/aad37f, https://arxiv.org/abs/1805.01484 https://arxiv.org/abs/arXiv:1805.01484 [astro-ph.GA]

  76. [84]

    150(6):166

    Jura M (2015) Lambda Boo Abundance Patterns: Accretion from Orbiting Sources . 150(6):166. doi:10.1088/0004-6256/150/6/166, https://arxiv.org/abs/1509.04672 https://arxiv.org/abs/arXiv:1509.04672 [astro-ph.SR]

  77. [85]

    Meteoritics & Planetary Science 59(12):3193--3214

    Jurewicz AJG, Amarsi AM, Burnett DS, et al (2024) Differences in elemental abundances between CI chondrites and the solar photosphere . Meteoritics & Planetary Science 59(12):3193--3214. doi:10.1111/maps.14272

  78. [86]

    335(2):L45--L49

    Kamp I, Paunzen E (2002) The Bootis phenomenon: interaction between a star and a diffuse interstellar cloud . 335(2):L45--L49. doi:10.1046/j.1365-8711.2002.05883.x, https://arxiv.org/abs/astro-ph/0207462 https://arxiv.org/abs/arXiv:astro-ph/0207462 [astro-ph]

  79. [87]

    91(1-2):175--180

    Kippenhahn R, Ruschenplatt G, Thomas HC (1980) The time scale of thermohaline mixing in stars . 91(1-2):175--180

  80. [88]

    An investigation with SST/TRIPPEL

    Kiselman D, Pereira TMD, Gustafsson B, et al (2011) Is the solar spectrum latitude-dependent?. An investigation with SST/TRIPPEL . 535:A14. doi:10.1051/0004-6361/201117553, https://arxiv.org/abs/1108.4527 https://arxiv.org/abs/arXiv:1108.4527 [astro-ph.SR]

  81. [89]

    Korn AJ, Grundahl F, Richard O, et al (2007) Atomic Diffusion and Mixing in Old Stars. I. Very Large Telescope FLAMES-UVES Observations of Stars in NGC 6397 . 671(1):402--419. doi:10.1086/523098, https://arxiv.org/abs/0709.0639 https://arxiv.org/abs/arXiv:0709.0639 [astro-ph]

  82. [90]

    doi:10.1002/chem.201801847

    Krishnamurthy R (2018) Life's Biological Chemistry: A Destiny or Destination Starting from Prebiotic Chemistry? Chemistry - A European Journal 24(63):16,708--16,715. doi:10.1002/chem.201801847

  83. [91]

    Kubryk M, Prantzos N, Athanassoula E (2015) Evolution of the Milky Way with radial motions of stars and gas. I. The solar neighbourhood and the thin and thick disks . 580:A126. doi:10.1051/0004-6361/201424171, https://arxiv.org/abs/1412.0585 https://arxiv.org/abs/arXiv:1412.05...

  84. [92]

    846(1):7

    Kuffmeier M, Haugb lle T, Nordlund A (2017) Zoom-in Simulations of Protoplanetary Disks Starting from GMC Scales . 846(1):7. doi:10.3847/1538-4357/aa7c64, https://arxiv.org/abs/1611.10360 https://arxiv.org/abs/arXiv:1611.10360 [astro-ph.SR]

  85. [93]

    Kunitomo M, Guillot T, Takeuchi T, et al (2017) Revisiting the pre-main-sequence evolution of stars. I. Importance of accretion efficiency and deuterium abundance . 599:A49. doi:10.1051/0004-6361/201628260, https://arxiv.org/abs/1702.07901 https://arxiv.org/abs/arXiv:1702.0790...

  86. [94]

    Kunitomo M, Guillot T, Ida S, et al (2018) Revisiting the pre-main-sequence evolution of stars. II. Consequences of planet formation on stellar surface composition . 618:A132. doi:10.1051/0004-6361/201833127, https://arxiv.org/abs/1808.07396 https://arxiv.org/abs/arXiv:1808.07...

  87. [95]

    533(1):538--550

    Lehmann C, Feltzing S, Feuillet D, et al (2024) Probing the strength of radial migration via churning by using metal-rich red giant stars from APOGEE . 533(1):538--550. doi:10.1093/mnras/stae1736, https://arxiv.org/abs/2405.19089 https://arxiv.org/abs/arXiv:2405.19089 [astro-ph.GA]

  88. [96]

    Treatise on Geochemistry 7:51--112

    Lichtenberg T, Miguel Y (2025) Super-Earths and Earth-like Exoplanets . Treatise on Geochemistry 7:51--112. doi:10.1016/B978-0-323-99762-1.00122-4, https://arxiv.org/abs/2405.04057 https://arxiv.org/abs/arXiv:2405.04057 [astro-ph.EP]

  89. [97]

    62(1):475--527

    Lind K, Amarsi AM (2024) Three-Dimensional Nonlocal Thermodynamic Equilibrium Abundance Analyses of Late-Type Stars . 62(1):475--527. doi:10.1146/annurev-astro-052722-103557, https://arxiv.org/abs/2401.00697 https://arxiv.org/abs/arXiv:2401.00697 [astro-ph.SR]

  90. [98]

    463(1):696--704

    Liu F, Asplund M, Yong D, et al (2016 a ) The chemical compositions of solar twins in the open cluster M67 . 463(1):696--704. doi:10.1093/mnras/stw2045, https://arxiv.org/abs/1608.03788 https://arxiv.org/abs/arXiv:1608.03788 [astro-ph.SR]

  91. [99]

    457(4):3934--3948

    Liu F, Yong D, Asplund M, et al (2016 b ) The Hyades open cluster is chemically inhomogeneous . 457(4):3934--3948. doi:10.1093/mnras/stw247, https://arxiv.org/abs/1601.07354 https://arxiv.org/abs/arXiv:1601.07354 [astro-ph.SR]

  92. [100]

    627:A117

    Liu F, Asplund M, Yong D, et al (2019) Chemical (in)homogeneity and atomic diffusion in the open cluster M 67 . 627:A117. doi:10.1051/0004-6361/201935306, https://arxiv.org/abs/1902.11008 https://arxiv.org/abs/arXiv:1902.11008 [astro-ph.SR]

  93. [101]

    508(1):1227--1240

    Liu F, Bitsch B, Asplund M, et al (2021) Detailed elemental abundances of binary stars: searching for signatures of planet formation and atomic diffusion . 508(1):1227--1240. doi:10.1093/mnras/stab2471, https://arxiv.org/abs/2108.11001 https://arxiv.org/abs/arXiv:2108.11001 [a...

  94. [102]

    627(8004):501--504

    Liu F, Ting YS, Yong D, et al (2024) At least one in a dozen stars shows evidence of planetary ingestion . 627(8004):501--504. doi:10.1038/s41586-024-07091-y, https://arxiv.org/abs/2403.13209 https://arxiv.org/abs/arXiv:2403.13209 [astro-ph.SR]

  95. [103]

    591(2):1220--1247

    Lodders K (2003) Solar System Abundances and Condensation Temperatures of the Elements . 591(2):1220--1247. doi:10.1086/375492

  96. [104]

    221(2):23

    Lodders K, Bergemann M, Palme H (2025) Solar System Elemental Abundances from the Solar Photosphere and CI-Chondrites . 221(2):23. doi:10.1007/s11214-025-01146-w, https://arxiv.org/abs/2502.10575 https://arxiv.org/abs/arXiv:2502.10575 [astro-ph.SR]

  97. [105]

    652(2):1755--1762

    Looney LW, Tobin JJ, Fields BD (2006) Radioactive Probes of the Supernova-contaminated Solar Nebula: Evidence that the Sun Was Born in a Cluster . 652(2):1755--1762. doi:10.1086/508407, https://arxiv.org/abs/astro-ph/0608411 https://arxiv.org/abs/arXiv:astro-ph/0608411 [astro-ph]

  98. [106]

    The age-chromospheric activity relation

    Lorenzo-Oliveira D, Freitas FC, Mel \'e ndez J, et al (2018) The Solar Twin Planet Search. The age-chromospheric activity relation . 619:A73. doi:10.1051/0004-6361/201629294, https://arxiv.org/abs/1806.08014 https://arxiv.org/abs/arXiv:1806.08014 [astro-ph.SR]

  99. [107]

    In: Evans DS, Wills D, Wills BJ (eds) External Galaxies and Quasi-Stellar Objects, p 56

    Lynds BT (1972) Distribution of Dust and HII Regions of Spiral Galaxies . In: Evans DS, Wills D, Wills BJ (eds) External Galaxies and Quasi-Stellar Objects, p 56

  100. [108]

    Magg E, Bergemann M, Serenelli A, et al (2022) Observational constraints on the origin of the elements. IV. Standard composition of the Sun . 661:A140. doi:10.1051/0004-6361/202142971, https://arxiv.org/abs/2203.02255 https://arxiv.org/abs/arXiv:2203.02255 [astro-ph.SR]

  101. [109]

    628:A126

    Maia MT, Mel \'e ndez J, Lorenzo-Oliveira D, et al (2019) Revisiting the 16 Cygni planet host at unprecedented precision and exploring automated tools for precise abundances . 628:A126. doi:10.1051/0004-6361/201935952, https://arxiv.org/abs/1906.04195 https://arxiv.org/abs/arX...

  102. [110]

    Matsuno T, Amarsi AM, Carlos M, et al (2024) 3D non-local thermodynamic equilibrium magnesium abundances reveal a distinct halo population . 688:A72. doi:10.1051/0004-6361/202450057, https://arxiv.org/abs/2405.13486 https://arxiv.org/abs/arXiv:2405.13486 [astro-ph.SR]

  103. [111]

    Matteucci F (2021) Modelling the chemical evolution of the Milky Way . 29(1):5. doi:10.1007/s00159-021-00133-8, https://arxiv.org/abs/2106.13145 https://arxiv.org/abs/arXiv:2106.13145 [astro-ph.GA]

  104. [112]

    Numerical simulation of the nearly Jeans-unstable case

    Mattsson L, Hedvall R (2022) Acceleration and clustering of cosmic dust in a gravoturbulent gas I. Numerical simulation of the nearly Jeans-unstable case . 509(3):3660--3676. doi:10.1093/mnras/stab3216, https://arxiv.org/abs/2111.01289 https://arxiv.org/abs/arXiv:2111.01289 [a...

  105. [113]

    641(2):L133--L136

    Mel \'e ndez J, Dodds-Eden K, Robles JA (2006) HD 98618: A Star Closely Resembling Our Sun . 641(2):L133--L136. doi:10.1086/503898, https://arxiv.org/abs/astro-ph/0603219 https://arxiv.org/abs/arXiv:astro-ph/0603219 [astro-ph]

  106. [114]

    704(1):L66--L70

    Mel \'e ndez J, Asplund M, Gustafsson B, et al (2009) The Peculiar Solar Composition and Its Possible Relation to Planet Formation . 704(1):L66--L70. doi:10.1088/0004-637X/704/1/L66, https://arxiv.org/abs/0909.2299 https://arxiv.org/abs/arXiv:0909.2299 [astro-ph.SR]

  107. [115]

    Mel \'e ndez J, Asplund M, Gustafsson B, et al (2010) Unprecedented accurate abundances: signatures of other Earths? In: Cunha K, Spite M, Barbuy B (eds) Chemical Abundances in the Universe: Connecting First Stars to Planets, pp 412--415, doi:10.1017/S1743921310001109, 0910.0875

  108. [116]

    doi:10.1007/978-3-319-19854-5

    Michaud G, Alecian G, Richer J (2015) Atomic Diffusion in Stars . doi:10.1007/978-3-319-19854-5

  109. [117]

    Miquelarena P, Saffe C, Flores M, et al (2024) The largest metallicity difference in twin systems: High-precision abundance analysis of the benchmark pair Krios and Kronos . 688:A73. doi:10.1051/0004-6361/202449983, https://arxiv.org/abs/2406.06705 https://arxiv.org/abs/arXiv:...

  110. [118]

    888(1):L9

    Nagar T, Spina L, Karakas AI (2020) The Chemical Signatures of Planetary Engulfment Events in Binary Systems . 888(1):L9. doi:10.3847/2041-8213/ab5dc6

  111. [119]

    907(2):116

    Nibauer J, Baxter EJ, Jain B, et al (2021) Statistics of the Chemical Composition of Solar Analog Stars and Links to Planet Formation . 907(2):116. doi:10.3847/1538-4357/abd0f1, https://arxiv.org/abs/2010.07241 https://arxiv.org/abs/arXiv:2010.07241 [astro-ph.SR]

  112. [120]

    Trends with stellar age and elemental condensation temperature

    Nissen PE (2015) High-precision abundances of elements in solar twin stars. Trends with stellar age and elemental condensation temperature . 579:A52. doi:10.1051/0004-6361/201526269, https://arxiv.org/abs/1504.07598 https://arxiv.org/abs/arXiv:1504.07598 [astro-ph.SR]

  113. [121]

    Trends of element ratios with stellar age

    Nissen PE (2016) High-precision abundances of Sc, Mn, Cu, and Ba in solar twins. Trends of element ratios with stellar age . 593:A65. doi:10.1051/0004-6361/201628888, https://arxiv.org/abs/1606.08399 https://arxiv.org/abs/arXiv:1606.08399 [astro-ph.SR]

  114. [122]

    Nissen PE, Gustafsson B (2018) High-precision stellar abundances of the elements: methods and applications . 26(1):6. doi:10.1007/s00159-018-0111-3, https://arxiv.org/abs/1810.06535 https://arxiv.org/abs/arXiv:1810.06535 [astro-ph.SR]

  115. [123]

    Verification of trends with stellar age

    Nissen PE, Silva Aguirre V, Christensen-Dalsgaard J, et al (2017) High-precision abundances of elements in Kepler LEGACY stars. Verification of trends with stellar age . 608:A112. doi:10.1051/0004-6361/201731845, https://arxiv.org/abs/1710.03544 https://arxiv.org/abs/arXiv:171...

  116. [124]

    Evidence of two distinct sequences in abundance-age relations

    Nissen PE, Christensen-Dalsgaard J, Mosumgaard JR, et al (2020) High-precision abundances of elements in solar-type stars. Evidence of two distinct sequences in abundance-age relations . 640:A81. doi:10.1051/0004-6361/202038300, https://arxiv.org/abs/2006.06013 https://arxiv.o...

  117. [125]

    Nuclear Physics A 777:424--458

    Nomoto K, Tominaga N, Umeda H, et al (2006) Nucleosynthesis yields of core-collapse supernovae and hypernovae, and galactic chemical evolution . Nuclear Physics A 777:424--458. doi:10.1016/j.nuclphysa.2006.05.008, https://arxiv.org/abs/astro-ph/0605725 https://arxiv.org/abs/ar...

  118. [126]

    51(1):457--509

    Nomoto K, Kobayashi C, Tominaga N (2013) Nucleosynthesis in Stars and the Chemical Enrichment of Galaxies . 51(1):457--509. doi:10.1146/annurev-astro-082812-140956

  119. [127]

    603:A112

    Nordlander T, Rickman H, Gustafsson B (2017) The destruction of an Oort Cloud in a rich stellar cluster . 603:A112. doi:10.1051/0004-6361/201630342, https://arxiv.org/abs/1704.03341 https://arxiv.org/abs/arXiv:1704.03341 [astro-ph.EP]

  120. [128]

    Chemical abundance variations in the globular cluster M4 (NGC 6121)

    Nordlander T, Gruyters P, Richard O, et al (2024) Atomic diffusion and mixing in old stars - VIII. Chemical abundance variations in the globular cluster M4 (NGC 6121) . 527(4):12,120--12,139. doi:10.1093/mnras/stad3973, https://arxiv.org/abs/2312.09657 https://arxiv.org/abs/ar...

  121. [129]

    arXiv e-prints arXiv:2506.04199

    Nordlund A (2025) Abundance Effects from Protoplanetary Disk Outflows . arXiv e-prints arXiv:2506.04199. https://arxiv.org/abs/2506.04199 https://arxiv.org/abs/arXiv:2506.04199 [astro-ph.EP]

  122. [130]

    Oetjens A, Carone L, Bergemann M, et al (2020) The influence of planetary engulfment on stellar rotation in metal-poor main-sequence stars . 643:A34. doi:10.1051/0004-6361/202038653, https://arxiv.org/abs/2009.03624 https://arxiv.org/abs/arXiv:2009.03624 [astro-ph.SR]

  123. [131]

    854(2):138

    Oh S, Price-Whelan AM, Brewer JM, et al (2018) Kronos and Krios: Evidence for Accretion of a Massive, Rocky Planetary System in a Comoving Pair of Solar-type Stars . 854(2):138. doi:10.3847/1538-4357/aaab4d, https://arxiv.org/abs/1709.05344 https://arxiv.org/abs/arXiv:1709.053...

  124. [132]

    \"O nehag A, Korn A, Gustafsson B, et al (2011) M67-1194, an unusually Sun-like solar twin in M67 . 528:A85. doi:10.1051/0004-6361/201015138, https://arxiv.org/abs/1009.4579 https://arxiv.org/abs/arXiv:1009.4579 [astro-ph.SR]

  125. [133]

    562:A102

    \"O nehag A, Gustafsson B, Korn A (2014) Abundances and possible diffusion of elements in M 67 stars . 562:A102. doi:10.1051/0004-6361/201322663, https://arxiv.org/abs/1310.6297 https://arxiv.org/abs/arXiv:1310.6297 [astro-ph.SR]

  126. [134]

    266(3):379--387

    Paunzen E (1999) The Group Of Bootis Stars . 266(3):379--387. doi:10.1023/A:1002034129866

  127. [135]

    523(2):2126--2145

    Prantzos N, Abia C, Chen T, et al (2023) On the origin of the Galactic thin and thick discs, their abundance gradients and the diagnostic potential of their abundance ratios . 523(2):2126--2145. doi:10.1093/mnras/stad1551, https://arxiv.org/abs/2305.13431 https://arxiv.org/abs...

  128. [136]

    Ram \' rez I, Asplund M, Baumann P, et al (2010) A possible signature of terrestrial planet formation in the chemical composition of solar analogs . 521:A33. doi:10.1051/0004-6361/201014456, https://arxiv.org/abs/1008.3161 https://arxiv.org/abs/arXiv:1008.3161 [astro-ph.SR]

  129. [137]

    doi:10.1088/0004-637X/740/2/76, https://arxiv.org/abs/1107.5814 https://arxiv.org/abs/arXiv:1107.5814 [astro-ph.SR]

    Ram \' rez I, Mel \'e ndez J, Cornejo D, et al (2011) Elemental Abundance Differences in the 16 Cygni Binary System: A Signature of Gas Giant Planet Formation? 740(2):76. doi:10.1088/0004-637X/740/2/76, https://arxiv.org/abs/1107.5814 https://arxiv.org/abs/arXiv:1107.5814 [ast...

  130. [138]

    756(1):46

    Ram \' rez I, Fish JR, Lambert DL, et al (2012) Lithium Abundances in nearby FGK Dwarf and Subgiant Stars: Internal Destruction, Galactic Chemical Evolution, and Exoplanets . 756(1):46. doi:10.1088/0004-637X/756/1/46, https://arxiv.org/abs/1207.0499 https://arxiv.org/abs/arXiv...

  131. [139]

    Ram \' rez I, Mel \'e ndez J, Asplund M (2014) Chemical signatures of planets: beyond solar-twins . 561:A7. doi:10.1051/0004-6361/201322558, https://arxiv.org/abs/1310.8581 https://arxiv.org/abs/arXiv:1310.8581 [astro-ph.SR]

  132. [140]

    808(1):13

    Ram \' rez I, Khanal S, Aleo P, et al (2015) The Dissimilar Chemical Composition of the Planet-hosting Stars of the XO-2 Binary System . 808(1):13. doi:10.1088/0004-637X/808/1/13, https://arxiv.org/abs/1506.01025 https://arxiv.org/abs/arXiv:1506.01025 [astro-ph.SR]

  133. [141]

    965(2):176

    Rampalli R, Ness MK, Edwards GH, et al (2024) The Sun Remains Relatively Refractory Depleted: Elemental Abundances for 17,412 Gaia RVS Solar Analogs and 50 Planet Hosts . 965(2):176. doi:10.3847/1538-4357/ad303e, https://arxiv.org/abs/2402.16954 https://arxiv.org/abs/arXiv:240...

  134. [142]

    In: Complex Planetary Systems, Proceedings of the International Astronomical Union, pp 194--203, doi:10.1017/S1743921314008254, 1409.6340

    Raymond SN, Morbidelli A (2014) The Grand Tack model: a critical review . In: Complex Planetary Systems, Proceedings of the International Astronomical Union, pp 194--203, doi:10.1017/S1743921314008254, 1409.6340

  135. [143]

    ://www.amazon.com/Quotations-Baker-Street-George-Vanderburgh/dp/1896032168

    Redmond C (1994) Quotations from Baker Street. ://www.amazon.com/Quotations-Baker-Street-George-Vanderburgh/dp/1896032168

  136. [144]

    Science 368(6490):518--521

    Reinhold T, Shapiro AI, Solanki SK, et al (2020) The Sun is less active than other solar-like stars . Science 368(6490):518--521. doi:10.1126/science.aay3821, https://arxiv.org/abs/2005.01401 https://arxiv.org/abs/arXiv:2005.01401 [astro-ph.SR]

  137. [145]

    In: Alecian G, Richard O, Vauclair S (eds) EAS Publications Series, pp 43--52, doi:10.1051/eas:2005097

    Richard O (2005) Evolutionary stellar models including diffusion and radiative accelerations . In: Alecian G, Richard O, Vauclair S (eds) EAS Publications Series, pp 43--52, doi:10.1051/eas:2005097

  138. [146]

    619(1):538--548

    Richard O, Michaud G, Richer J (2005) Implications of WMAP Observations on Li Abundance and Stellar Evolution Models . 619(1):538--548. doi:10.1086/426470, https://arxiv.org/abs/astro-ph/0409672 https://arxiv.org/abs/arXiv:astro-ph/0409672 [astro-ph]

  139. [147]

    Implications for chemical tagging studies

    Saffe C, Jofr \'e E, Martioli E, et al (2017) Signatures of rocky planet engulfment in HAT-P-4. Implications for chemical tagging studies . 604:L4. doi:10.1051/0004-6361/201731430, https://arxiv.org/abs/1707.02180 https://arxiv.org/abs/arXiv:1707.02180 [astro-ph.SR]

  140. [148]

    506(1):L65--L68

    Sandquist E, Taam RE, Lin DNC, et al (1998) Planet Consumption and Stellar Metallicity Enhancements . 506(1):L65--L68. doi:10.1086/311633, https://arxiv.org/abs/astro-ph/9808128 https://arxiv.org/abs/arXiv:astro-ph/9808128 [astro-ph]

  141. [149]

    572(2):1012--1023

    Sandquist EL, Dokter JJ, Lin DNC, et al (2002) A Critical Examination of Li Pollution and Giant-Planet Consumption by a Host Star . 572(2):1012--1023. doi:10.1086/340452, https://arxiv.org/abs/astro-ph/0202527 https://arxiv.org/abs/arXiv:astro-ph/0202527 [astro-ph]

  142. [150]

    373:1019--1031

    Santos NC, Israelian G, Mayor M (2001) The metal-rich nature of stars with planets . 373:1019--1031. doi:10.1051/0004-6361:20010648, https://arxiv.org/abs/astro-ph/0105216 https://arxiv.org/abs/arXiv:astro-ph/0105216 [astro-ph]

  143. [151]

    J Comput Phys 59:56--80

    Scharmer GB, Carlsson M (1985) A new approach to multi-level non-LTE radiative transfer problems . J Comput Phys 59:56--80. doi:10.1016/0021-9991(85)90107-X

  144. [152]

    643:A164

    Semenova E, Bergemann M, Deal M, et al (2020) The Gaia-ESO survey: 3D NLTE abundances in the open cluster NGC 2420 suggest atomic diffusion and turbulent mixing are at the origin of chemical abundance variations . 643:A164. doi:10.1051/0004-6361/202038833, https://arxiv.org/ab...

  145. [153]

    Serenelli AM, Haxton WC, Pe \ n a-Garay C (2011) Solar Models with Accretion. I. Application to the Solar Abundance Problem . 743(1):24. doi:10.1088/0004-637X/743/1/24, https://arxiv.org/abs/1104.1639 https://arxiv.org/abs/arXiv:1104.1639 [astro-ph.SR]

  146. [154]

    516(3):3354--3365

    Sevilla J, Behmard A, Fuller J (2022) Long-term lithium abundance signatures following planetary engulfment . 516(3):3354--3365. doi:10.1093/mnras/stac2436, https://arxiv.org/abs/2207.13232 https://arxiv.org/abs/arXiv:2207.13232 [astro-ph.SR]

  147. [155]

    904(2):163

    Sieverding A, M \"u ller B, Qian YZ (2020) Nucleosynthesis of an 11.8 M _ Supernova with 3D Simulation of the Inner Ejecta: Overall Yields and Implications for Short-lived Radionuclides in the Early Solar System . 904(2):163. doi:10.3847/1538-4357/abc61b, https://arxiv.org/abs...

  148. [156]

    Snaith O, Haywood M, Di Matteo P, et al (2015) Reconstructing the star formation history of the Milky Way disc(s) from chemical abundances . 578:A87. doi:10.1051/0004-6361/201424281, https://arxiv.org/abs/1410.3829 https://arxiv.org/abs/arXiv:1410.3829 [astro-ph.GA]

  149. [157]

    arXiv e-prints arXiv:2408.15326

    Soliman NH, Hopkins PF (2024) Are Stars Really Ingesting their Planets? Examining an Alternative Explanation . arXiv e-prints arXiv:2408.15326. doi:10.48550/arXiv.2408.15326, https://arxiv.org/abs/2408.15326 https://arxiv.org/abs/arXiv:2408.15326 [astro-ph.GA]

  150. [158]

    arXiv e-prints arXiv:2406.09602

    Soliman NH, Hopkins PF, Grudi \'c MY (2024) Dust-Evacuated Zones Near Massive Stars: Consequences of Dust Dynamics on Star-forming Regions . arXiv e-prints arXiv:2406.09602. doi:10.48550/arXiv.2406.09602, https://arxiv.org/abs/2406.09602 https://arxiv.org/abs/arXiv:2406.09602 ...

  151. [159]

    895(1):52

    Spina L, Nordlander T, Casey AR, et al (2020) How Magnetic Activity Alters What We Learn from Stellar Spectra . 895(1):52. doi:10.3847/1538-4357/ab8bd7, https://arxiv.org/abs/2004.09771 https://arxiv.org/abs/arXiv:2004.09771 [astro-ph.SR]

  152. [160]

    Nature Astronomy 5:1163--1169

    Spina L, Sharma P, Mel \'e ndez J, et al (2021) Chemical evidence for planetary ingestion in a quarter of Sun-like stars . Nature Astronomy 5:1163--1169. doi:10.1038/s41550-021-01451-8, https://arxiv.org/abs/2108.12040 https://arxiv.org/abs/arXiv:2108.12040 [astro-ph.SR]

  153. [161]

    13:133--164

    Spitzer JL., Jenkins EB (1975) Ultraviolet studies of the interstellar gas. 13:133--164. doi:10.1146/annurev.aa.13.090175.001025

  154. [162]

    Stammler SM, Lichtenberg T, Dr a z kowska J, et al (2023) Leaky dust traps: How fragmentation impacts dust filtering by planets . 670:L5. doi:10.1051/0004-6361/202245512, https://arxiv.org/abs/2301.05505 https://arxiv.org/abs/arXiv:2301.05505 [astro-ph.EP]

  155. [163]

    Steffen M, Prakapavi c ius D, Caffau E, et al (2015) The photospheric solar oxygen project. IV. 3D-NLTE investigation of the 777 nm triplet lines . 583:A57. doi:10.1051/0004-6361/201526406, https://arxiv.org/abs/1508.03487 https://arxiv.org/abs/arXiv:1508.03487 [astro-ph.SR]

  156. [164]

    Stein RF, Nordlund A (1998) Simulations of Solar Granulation. I. General Properties . 499(2):914--933. doi:10.1086/305678

  157. [165]

    Proceedings of the National Academy of Science 52(2):387--397

    Suess HE (1964) On Element Synthesis and the Interpretation of the Abundances of Heavy Nuclides . Proceedings of the National Academy of Science 52(2):387--397. doi:10.1073/pnas.52.2.387

  158. [166]

    819(1):19

    Teske JK, Khanal S, Ram \' rez I (2016) The Curious Case of Elemental Abundance Differences in the Dual Hot Jupiter Hosts WASP-94A and B . 819(1):19. doi:10.3847/0004-637X/819/1/19, https://arxiv.org/abs/1601.01731 https://arxiv.org/abs/arXiv:1601.01731 [astro-ph.SR]

  159. [167]

    744(2):123

    Th \'e ado S, Vauclair S (2012) Metal-rich Accretion and Thermohaline Instabilities in Exoplanet-host Stars: Consequences on the Light Elements Abundances . 744(2):123. doi:10.1088/0004-637X/744/2/123, https://arxiv.org/abs/1109.4238 https://arxiv.org/abs/arXiv:1109.4238 [astro-ph.SR]

  160. [168]

    doi:10.1093/mnrasl/slx096, https://arxiv.org/abs/1706.05107 https://arxiv.org/abs/arXiv:1706.05107 [astro-ph.GA]

    Tricco TS, Price DJ, Laibe G (2017) Is the dust-to-gas ratio constant in molecular clouds? 471(1):L52--L56. doi:10.1093/mnrasl/slx096, https://arxiv.org/abs/1706.05107 https://arxiv.org/abs/arXiv:1706.05107 [astro-ph.GA]

  161. [169]

    904(2):137

    Tsujimoto T, Baba J (2020) Remarkable Migration of the Solar System from the Innermost Galactic Disk; a Wander, a Wobble, and a Climate Catastrophe on the Earth . 904(2):137. doi:10.3847/1538-4357/abc00a, https://arxiv.org/abs/2010.05962 https://arxiv.org/abs/arXiv:2010.05962 ...

  162. [170]

    863(2):L27

    Tsujimoto T, Nishimura N (2018) Early Chemical Evolution of Zn Driven by Magnetorotational Supernovae and the Pathway to the Solar Zn Composition . 863(2):L27. doi:10.3847/2041-8213/aad86b, https://arxiv.org/abs/1808.02524 https://arxiv.org/abs/arXiv:1808.02524 [astro-ph.GA]

  163. [171]

    Ulrich RK (1972) Thermohaline Convection in Stellar Interiors. 172:165. doi:10.1086/151336

  164. [172]

    Venn KA, Lambert DL (1990) The Chemical Composition of Three Lambda Bootis Stars . 363:234. doi:10.1086/169334

  165. [173]

    The role of non-radial radiation pressure in dust dynamics

    Vinkovi \'c D, C emelji \'c M (2024) Inner dusty regions of protoplanetary discs - III. The role of non-radial radiation pressure in dust dynamics . 532(2):2388--2400. doi:10.1093/mnras/stae1635, https://arxiv.org/abs/2407.15265 https://arxiv.org/abs/arXiv:2407.15265 [astro-ph.EP]

  166. [174]

    Vorobyov EI, Elbakyan V, Hosokawa T, et al (2017) Effect of accretion on the pre-main-sequence evolution of low-mass stars and brown dwarfs . 605:A77. doi:10.1051/0004-6361/201630356, https://arxiv.org/abs/1706.00502 https://arxiv.org/abs/arXiv:1706.00502 [astro-ph.SR]

  167. [175]

    482(2):2222--2233

    Wang HS, Liu F, Ireland TR, et al (2019) Enhanced constraints on the interior composition and structure of terrestrial exoplanets . 482(2):2222--2233. doi:10.1093/mnras/sty2749, https://arxiv.org/abs/1810.04615 https://arxiv.org/abs/arXiv:1810.04615 [astro-ph.EP]

  168. [176]

    Waters LBFM, Trams NR, Waelkens C (1992) A scenario for the selective depletion of stellar atmospheres. 262:L37

  169. [177]

    Wielen R, Fuchs B, Dettbarn C (1996) On the birth-place of the Sun and the places of formation of other nearby stars . 314:438

  170. [178]

    Astronomy and Geophysics 65(3):3.18--3.22

    Wilson A, Walker A, Alf \`e D, et al (2024) Solid-Liquid Interactions in Deep Planetary Interiors . Astronomy and Geophysics 65(3):3.18--3.22. doi:10.1093/astrogeo/atae036

  171. [179]

    586(7830):528--532

    Winter AJ, Kruijssen JMD, Longmore SN, et al (2020) Stellar clustering shapes the architecture of planetary systems . 586(7830):528--532. doi:10.1038/s41586-020-2800-0, https://arxiv.org/abs/2010.10531 https://arxiv.org/abs/arXiv:2010.10531 [astro-ph.EP]

  172. [180]

    High precision stellar parameters for 250 stars

    Yong D, Liu F, Ting YS, et al (2023) C3PO: towards a complete census of co-moving pairs of stars - I. High precision stellar parameters for 250 stars . 526(2):2181--2195. doi:10.1093/mnras/stad2679, https://arxiv.org/abs/2309.01546 https://arxiv.org/abs/arXiv:2309.01546 [astro-ph.SR]

  173. [181]

    Earth and Planetary Science Letters 392:16--27

    Young ED (2014) Inheritance of solar short- and long-lived radionuclides from molecular clouds and the unexceptional nature of the solar system . Earth and Planetary Science Letters 392:16--27. doi:10.1016/j.epsl.2014.02.014, https://arxiv.org/abs/1403.0832 https://arxiv.org/a...

  174. [182]

    doi:10.1093/mnras/staf436, https://arxiv.org/abs/2503.10339 https://arxiv.org/abs/arXiv:2503.10339 [astro-ph.EP]

    Yu J, Ting YS, Casagrande L, et al (2025) C3PO IV: co-natal stars depleted in refractories are magnetically more active - possible imprints of planets . doi:10.1093/mnras/staf436, https://arxiv.org/abs/2503.10339 https://arxiv.org/abs/arXiv:2503.10339 [astro-ph.EP]

  175. [183]

    Zuckerman B, Evans IN. J. (1974) Models of Massive Molecular Clouds . 192:L149. doi:10.1086/181613

  176. [184]

    462(2):795--799

    Zwitter T, Mignard F, Crifo F (2007) Asteroids as radial velocity and resolving power standards for medium and high resolution spectroscopy . 462(2):795--799. doi:10.1051/0004-6361:20053717, https://arxiv.org/abs/astro-ph/0609110 https://arxiv.org/abs/arXiv:astro-ph/0609110 [astro-ph]

Pith tools

Reviewed August 5, 2026 · model on record in the stance chip above.