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arxiv: 2606.31218 · v1 · pith:H2YPW5ZUnew · submitted 2026-06-30 · 🌌 astro-ph.GA

The Sc, Ti, and V Abundance Discrepancy: Testing High-Mass IMF Variation and Massive-Star Rotation

Soonchul Choi , Eda Gjergo , Youngman Kim , Toshitaka Kajino This is my paper

Pith reviewed 2026-07-01 05:08 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords galactic chemical evolutionmassive starsstellar rotationinitial mass functionscandiumtitaniumvanadiummetal-poor stars
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The pith

Rotating massive-star yields at 300 km/s bring Sc, Ti, and V model trends closer to metal-poor halo observations.

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

The paper examines why Galactic chemical evolution models underproduce scandium, titanium, and vanadium at early times. It runs a grid of one-zone models that change the initial rotational velocity of massive stars and the high-mass slope of the initial mass function. Models using yields from stars rotating at 300 km/s match the observed [X/Fe] trends better, especially below [Fe/H] = -2. Changing the initial mass function slope gives only secondary shifts. Discrepancies that remain at higher metallicities point to the need for more complete yield and enrichment treatments.

Core claim

Adopting rotating massive-star yields with an initial rotational velocity of 300 km/s brings the model trends closer to metal-poor observations, especially for halo stars ([Fe/H] < -2), and improves the joint behavior of Sc, Ti, and V. Variations of the high-mass slope of the initial mass function produce a secondary modulation.

What carries the argument

A grid of one-zone Galactic chemical evolution models that varies massive-star initial rotational velocity and the high-mass IMF slope, then compares the resulting [X/Fe] versus [Fe/H] tracks and cross-element correlations to Galactic abundance data.

If this is right

  • Rotating yields at 300 km/s improve agreement with halo-star data for all three elements simultaneously.
  • IMF slope changes modulate the same trends but do not remove the main mismatch.
  • Tensions persist at solar and super-solar metallicities, indicating missing physics beyond rotation and IMF shape.
  • The joint Sc-Ti-V behavior is a stronger test than any single element.

Where Pith is reading between the lines

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

  • Rotation may be a dominant factor in the earliest enrichment of the Galactic halo.
  • Similar yield adjustments could affect predictions for neighboring elements produced in the same stars.
  • Extending the models to include binary evolution or variable star-formation rates would test whether rotation remains the leading fix.
  • Surveys that deliver uniform Sc-Ti-V data across metallicities could isolate the rotation signal from observational scatter.

Load-bearing premise

The Sc, Ti, and V abundance discrepancies are driven primarily by changes in massive-star yields rather than by other enrichment channels, selection effects, or the limits of the one-zone setup.

What would settle it

New high-precision abundance measurements for Sc, Ti, and V in a large sample of halo stars at [Fe/H] < -2 that still show the same underproduction even after the rotating yields are adopted.

Figures

Figures reproduced from arXiv: 2606.31218 by Eda Gjergo, Soonchul Choi, Toshitaka Kajino, Youngman Kim.

Figure 1
Figure 1. Figure 1: presents the IMF for different high-mass slopes, α3 = 1.6, 2.3, and 3.0, over the stellar mass range of 0.08 to 120M⊙. The normalization is chosen such that the integral of the mass-weighted IMF is unity (Eq. 2). As α3 increases, the IMF becomes steeper at the mas￾sive star, resulting in a lower fraction of massive stars. Since these stars are the primary sites for the synthesis of elements such as Sc, Ti,… view at source ↗
Figure 2
Figure 2. Figure 2: Isotope yields of Sc, Ti, and V from a 13M⊙ star at various metallicities ([Z] = log10(Z/Z⊙)). The yields are taken from M. Limongi & A. Chieffi (2018). Different markers refer to different initial rotational velocities (IRV). The panels correspond to the following metallicities: [Z] = 0 (top-left), [Z] = −1 (top-right), [Z] = −2 (bottom-left), and [Z] = −3 (bottom-right). For visual clarity, isotopes of t… view at source ↗
Figure 3
Figure 3. Figure 3: Four-panel comparison of the one-zone GCE histories for three high-mass IMF slopes, α3 = 1.6, 2.3, and 3.0, using the non-rotating massive-star yield set (IRV = 0 km/s). From left to right, the panels show the total stellar mass together with the metal-enriched gas mass, the CCSN mass-return rate, the AGB mass-return rate, and the star-formation rate. In the first panel, the dotted purple line denotes the … view at source ↗
Figure 4
Figure 4. Figure 4: The abundance ratios [X/Fe] (where X = Sc, Ti, and V) as a function of [Fe/H] for different values of the IMF slope parameter, α3. The massive-star yields correspond to the non-rotating case, i.e., IRV = 0 km/s. Observational point colours follow the literature subsamples defined in Section 2. Blue denotes studies containing both thin- and thick-disc stars, red denotes halo-only samples, black denotes thin… view at source ↗
Figure 5
Figure 5. Figure 5: Returned masses as functions of [Fe/H] for Na, Mg, Al, Sc, Ti, V, and Fe for the three IMF slopes. Here “returned mass” denotes the mass of a given element released to the ISM by the indicated source at the model step corresponding to that [Fe/H]. The three stacked panels show the contributions from AGB stars (top), CCSNe (middle), and SNe Ia (bottom). The massive-star yields are the non-rotating set, i.e.… view at source ↗
Figure 6
Figure 6. Figure 6: Ratio of the returned mass from CCSNe to that from AGB stars for different high-mass IMF slopes, α3 = 1.6, 2.3, and 3.0. The massive-star yields are the non-rotating set, i.e., IRV = 0 km/s. 4 2 0 10 3 10 4 10 5 10 6 10 7 10 8 10 9 10 10 10 11 M a s s e s [M ] Mstar MZ, g IRV = 0 km/s MZ, g IRV = 150 km/s MZ, g IRV = 300 km/s 4 2 0 10 3 10 2 10 1 10 0 R a t e s C C S N [M /y r] 3 = 2.3 4 2 0 10 3 10 2 10 1… view at source ↗
Figure 7
Figure 7. Figure 7: Four-panel comparison of the one-zone GCE histories for three representative initial rotational velocities (IRVs) of the massive-star models. From left to right, the panels show the total stellar mass together with the metal-enriched gas mass, the CCSN mass-return rate, the AGB mass-return rate, and the star-formation rate. In the first panel, the dotted purple line denotes the total stellar mass, Mstar. T… view at source ↗
Figure 8
Figure 8. Figure 8: The abundance ratios [X/Fe] (where X = Sc, Ti, and V) as a function of [Fe/H] for different values of IRV. The IMF slope is set at the canonical value, α3 = 2.3. Observational point colours follow the literature subsamples defined in Section 2. Blue denotes studies containing both thin- and thick-disc stars, red denotes halo-only samples, black denotes thin-disc-only samples, and green denotes mixed thick-… view at source ↗
Figure 9
Figure 9. Figure 9: Returned masses as functions of [Fe/H] for Na, Mg, Al, Sc, Ti, V, and Fe for the three representative IRVs, computed at a high-mass IMF slope of α3 = 2.3. Here “returned mass” denotes the mass of a given element released to the ISM by the indicated source at the model step corresponding to that [Fe/H]. The upper and lower panels show the AGB and CCSN contributions, respectively. suggesting that rapid rotat… view at source ↗
Figure 10
Figure 10. Figure 10: Ratio of the returned mass from CCSN to that from AGB for various IRVs, computed at a value of α3 = 2.3. In [PITH_FULL_IMAGE:figures/full_fig_p011_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: Four-panel comparison of the one-zone GCE histories for three high-mass IMF slopes at an initial rotational velocity IRV = 300 km/s. From left to right, the panels show the total stellar mass together with the metal-enriched gas mass, the CCSN mass-return rate, the AGB mass-return rate, and the star-formation rate. In the first panel, the dotted purple line denotes the total stellar mass, Mstar. Blue line… view at source ↗
Figure 12
Figure 12. Figure 12: Evolution of [Fe/H] as a function of Galaxy age for the combined-effect models shown in [PITH_FULL_IMAGE:figures/full_fig_p013_12.png] view at source ↗
Figure 13
Figure 13. Figure 13: The abundance ratios [X/Fe] (where X = Na, Mg, Al, Sc, Ti, and V) as a function of [Fe/H] for different values of α3 with IRV = 300 km/s. Observational point colours follow the literature subsamples defined in Section 2. Blue denotes studies containing both thin- and thick-disc stars, red denotes halo-only samples, black denotes thin-disc-only samples, and green denotes mixed thick-disc/halo samples. The … view at source ↗
Figure 14
Figure 14. Figure 14: Correlations among the observed abundances of Sc, Ti, and V. The left, middle, and right panels show [Sc/Fe] versus [Ti/Fe], [Sc/Fe] versus [V/Fe], and [V/Fe] versus [Ti/Fe], respectively. Observational data are color-coded by literature subsample, with blue for thick- and thin-disc samples, red for halo samples, black for thin-disc samples, and green for mixed thick-disc and halo samples. The full refere… view at source ↗
read the original abstract

Scandium, titanium, and vanadium can be synthesized primarily in massive stars. Yet many of the current Galactic chemical evolution models under-produce these elements at early epochs. Motivated by evidence that the initial mass function varied in the past on the Galactic disc, we examine how assumptions about massive-star rotation and the initial mass function affect the inferred evolution of Sc, Ti, and V. We compute a grid of one-zone Galactic chemical evolution models that varies the initial rotational velocity of massive stars and the high-mass slope of the initial mass function. We compare the resulting [X/Fe] vs [Fe/H] for X= Sc, Ti, and V tracks and cross-element correlations with Galactic abundance data. We find that adopting rotating massive-star yields with an initial rotational velocity of 300 km/s brings the model trends closer to metal-poor observations, especially for halo stars ([Fe/H] $< -2$), and improves the joint behavior of Sc, Ti, and V. Variations of the high-mass slope of the initial mass function produce a secondary modulation. The remaining tensions, most apparent at solar to super-solar metallicities, motivate future work with a more complete treatment of the enrichment physics and model uncertainties.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

3 major / 2 minor

Summary. The manuscript uses a grid of one-zone Galactic chemical evolution models to test how massive-star initial rotational velocity and high-mass IMF slope affect the predicted evolution of Sc, Ti, and V. It reports that yields with 300 km/s rotation bring the model [X/Fe] vs [Fe/H] tracks and cross-element correlations closer to metal-poor observations, especially halo stars at [Fe/H] < -2, while IMF slope variations provide only secondary modulation; remaining tensions at higher metallicities are noted as motivation for future work.

Significance. If the central claim holds, the work would indicate that stellar rotation is a key missing ingredient in early enrichment models for these elements. The systematic parameter grid is a positive methodological feature. However, the significance is reduced by the absence of quantitative fit metrics and by the use of one-zone models whose instantaneous-mixing assumption is particularly questionable for the halo regime highlighted in the claim.

major comments (3)
  1. [Abstract] Abstract: the reported improvement from 300 km/s rotation is stated only qualitatively, with no fit statistics, error bars on the model tracks, specification of the observational datasets, or exclusion criteria. This is load-bearing because the central claim rests on the assertion that the 300 km/s tracks are meaningfully closer to the data.
  2. [Results / halo comparison] Comparison to halo stars ([Fe/H] < -2): the one-zone models enforce instantaneous mixing and a single star-formation history, yet the manuscript does not test whether the 300 km/s preference survives when this assumption is relaxed (e.g., via multi-zone or inhomogeneous enrichment calculations). This directly affects the load-bearing claim for halo-star trends.
  3. [Results / parameter variation] Parameter selection: the 300 km/s value is identified because it improves agreement with observations, introducing circularity; no independent prior or blind-grid demonstration is provided to show that this velocity would have been preferred without reference to the data.
minor comments (2)
  1. [Abstract] The abstract refers to 'Galactic abundance data' without citing the specific catalog or reference used for the comparison.
  2. [Model description] Notation for abundance ratios and the precise definition of the high-mass IMF slope should be stated explicitly in the model-setup section for reproducibility.

Simulated Author's Rebuttal

3 responses · 1 unresolved

We thank the referee for their constructive comments on our manuscript. We provide point-by-point responses below and will revise the manuscript accordingly where feasible.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the reported improvement from 300 km/s rotation is stated only qualitatively, with no fit statistics, error bars on the model tracks, specification of the observational datasets, or exclusion criteria. This is load-bearing because the central claim rests on the assertion that the 300 km/s tracks are meaningfully closer to the data.

    Authors: We agree that quantitative support would strengthen the abstract. In revision we will specify the observational datasets (e.g., the metal-poor halo samples), report simple fit statistics such as mean absolute deviations between model tracks and binned data, note any exclusion criteria applied to the observations, and clarify the model uncertainties. revision: yes

  2. Referee: [Results / halo comparison] Comparison to halo stars ([Fe/H] < -2): the one-zone models enforce instantaneous mixing and a single star-formation history, yet the manuscript does not test whether the 300 km/s preference survives when this assumption is relaxed (e.g., via multi-zone or inhomogeneous enrichment calculations). This directly affects the load-bearing claim for halo-star trends.

    Authors: We acknowledge that the instantaneous-mixing assumption of one-zone models is a limitation for the halo regime. Our grid is designed as a controlled test within the standard one-zone framework; we will add explicit discussion of this caveat and qualify the halo-star claims accordingly, while noting multi-zone explorations as future work. revision: partial

  3. Referee: [Results / parameter variation] Parameter selection: the 300 km/s value is identified because it improves agreement with observations, introducing circularity; no independent prior or blind-grid demonstration is provided to show that this velocity would have been preferred without reference to the data.

    Authors: The 300 km/s rotation rate is a standard value drawn from existing massive-star yield grids in the literature and was included a priori in our systematic parameter exploration alongside the IMF slope. We will revise the text to clarify the physical motivation for this choice and the structure of the grid to reduce any appearance of post-hoc selection. revision: yes

standing simulated objections not resolved
  • Performing new multi-zone or inhomogeneous enrichment calculations to test whether the 300 km/s preference persists outside the one-zone assumption is outside the scope of the current study.

Circularity Check

1 steps flagged

300 km/s rotation velocity selected post-hoc to match data and reported as bringing trends closer

specific steps
  1. fitted input called prediction [Abstract]
    "We find that adopting rotating massive-star yields with an initial rotational velocity of 300 km/s brings the model trends closer to metal-poor observations, especially for halo stars ([Fe/H] < -2), and improves the joint behavior of Sc, Ti, and V."

    The 300 km/s value is identified from the grid precisely because it reduces the offset to observations; the reported 'improvement' therefore restates the selection criterion rather than deriving from independent first-principles yields or external constraints.

full rationale

The paper grids over initial rotational velocities and reports that 300 km/s improves agreement with metal-poor observations. This selection criterion makes the claimed improvement a direct consequence of choosing the parameter that minimizes the discrepancy, rather than an a priori prediction. No other circular steps (self-citation chains or definitional loops) are present in the provided text; the one-zone modeling assumptions are independent of this parameter choice.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The claim rests on standard one-zone GCE assumptions plus two varied parameters chosen to match data; no new entities are postulated.

free parameters (2)
  • initial rotational velocity of massive stars = 300 km/s
    Selected because it brings model trends closer to metal-poor observations
  • high-mass slope of the initial mass function
    Varied across a grid to test secondary modulation
axioms (2)
  • domain assumption One-zone models sufficiently capture the enrichment history of the Milky Way
    Framework used for all tracks without comparison to multi-zone or hydrodynamical alternatives
  • domain assumption Massive stars dominate production of Sc, Ti, and V
    Stated as motivation in the abstract

pith-pipeline@v0.9.1-grok · 5764 in / 1559 out tokens · 46385 ms · 2026-07-01T05:08:51.055584+00:00 · methodology

discussion (0)

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Reference graph

Works this paper leans on

99 extracted references · 70 canonical work pages · 44 internal anchors

  1. [1]

    The Messenger , volume=

    The Gaia-ESO public spectroscopic survey , author=. The Messenger , volume=

  2. [2]

    Publications of the Astronomical Society of the Pacific , volume=

    The apache point observatory galactic evolution experiment (apogee) spectrographs , author=. Publications of the Astronomical Society of the Pacific , volume=. 2019 , publisher=

    2019

  3. [3]

    Monthly Notices of the Royal Astronomical Society , volume=

    The GALAH+ survey: Third data release , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2021 , publisher=

    2021

  4. [4]

    The Astronomical Journal , volume=

    The radial velocity experiment (RAVE): first data release , author=. The Astronomical Journal , volume=. 2006 , publisher=

    2006

  5. [5]

    The Astronomical Journal , volume=

    SEGUE: A Spectroscopic Survey of 240,000 Stars with g= 14--20 , author=. The Astronomical Journal , volume=. 2009 , publisher=

    2009

  6. [6]

    Research in Astronomy and Astrophysics , volume=

    LAMOST Experiment for Galactic Understanding and Exploration (LEGUE)—The survey's science plan , author=. Research in Astronomy and Astrophysics , volume=. 2012 , publisher=

    2012

  7. [7]

    Francesca Matteucci , title =

  8. [8]

    Chemical abundances of 1111 FGK stars from the HARPS GTO planet search program.Galactic stellar populations and planets

    Chemical abundances of 1111 FGK stars from the HARPS GTO planet search program. Galactic stellar populations and planets. Astronomy & Astrophysics , keywords =. doi:10.1051/0004-6361/201219401 , archivePrefix =. 1207.2388 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201219401

  9. [9]

    The evolution of the C/O ratio in metal-poor halo stars

    The evolution of the C/O ratio in metal-poor halo stars. Astronomy & Astrophysics , keywords =. doi:10.1051/0004-6361:20034188 , archivePrefix =. astro-ph/0310472 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20034188

  10. [10]

    NLTE determination of the sodium abundance in a homogeneous sample of extremely metal-poor stars

    NLTE determination of the sodium abundance in a homogeneous sample of extremely metal-poor stars. Astronomy & Astrophysics , keywords =. doi:10.1051/0004-6361:20066232 , archivePrefix =. astro-ph/0701199 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20066232

  11. [11]

    NLTE determination of the aluminium abundance in a homogeneous sample of extremely metal-poor stars

    NLTE determination of the aluminium abundance in a homogeneous sample of extremely metal-poor stars. Astronomy & Astrophysics , keywords =. doi:10.1051/0004-6361:20078837 , archivePrefix =. 0802.1519 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20078837

  12. [12]

    Non-LTE abundances of Mg and K in extremely metal-poor stars and the evolution of [O/Mg], [Na/Mg], [Al/Mg] and [K/Mg] in the Milky Way

    Non-LTE abundances of Mg and K in extremely metal-poor stars and the evolution of [O/Mg], [Na/Mg], [Al/Mg], and [K/Mg] in the Milky Way. Astronomy & Astrophysics , keywords =. doi:10.1051/0004-6361/200913223 , archivePrefix =. 1001.1207 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/200913223

  13. [13]

    A., Primack, J

    The origin and chemical evolution of carbon in the Galactic thin and thick discs ^ *. Monthly Notices of the Royal Astronomical Society , keywords =. doi:10.1111/j.1365-2966.2006.10037.x , archivePrefix =. astro-ph/0601130 , primaryClass =

    work page doi:10.1111/j.1365-2966.2006.10037.x 2006

  14. [14]

    Exploring the Milky Way stellar disk. A detailed elemental abundance study of 714 F and G dwarf stars in the Solar neighbourhood

    Exploring the Milky Way stellar disk. A detailed elemental abundance study of 714 F and G dwarf stars in the solar neighbourhood. Astronomy & Astrophysics , keywords =. doi:10.1051/0004-6361/201322631 , archivePrefix =. 1309.2631 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201322631

  15. [15]

    Cu and Zn in the early Galaxy

    Cu and Zn in the early Galaxy. Astronomy & Astrophysics , keywords =. doi:10.1051/0004-6361:20035913 , archivePrefix =. astro-ph/0405050 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20035913

  16. [16]

    Sulphur abundance in Galactic stars

    Sulphur abundance in Galactic stars. Astronomy & Astrophysics , keywords =. doi:10.1051/0004-6361:20052905 , archivePrefix =. astro-ph/0507030 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20052905

  17. [17]

    The Galactic evolution of phosphorus

    The Galactic evolution of phosphorus. Astronomy & Astrophysics , keywords =. doi:10.1051/0004-6361/201117313 , archivePrefix =. 1107.2657 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201117313

  18. [18]

    Abundances of light elements in metal-poor stars. III. Data analysis and results. Astronomy & Astrophysics , keywords =

  19. [19]

    First stars V - Abundance patterns from C to Zn and supernova yields in the early Galaxy

    First stars V - Abundance patterns from C to Zn and supernova yields in the early Galaxy. Astronomy & Astrophysics , keywords =. doi:10.1051/0004-6361:20034074 , archivePrefix =. astro-ph/0311082 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20034074

  20. [20]

    The Chemical Evolution of the Draco Dwarf Spheroidal Galaxy

    The Chemical Evolution of the Draco Dwarf Spheroidal Galaxy. The Astrophysical Journal , keywords =. doi:10.1088/0004-637X/701/2/1053 , archivePrefix =. 0906.1006 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/701/2/1053

  21. [21]

    Normal and Outlying Populations of the Milky Way Stellar Halo at [Fe/H] < -2

    Normal and Outlying Populations of the Milky Way Stellar Halo at [Fe/H] <-2. The Astrophysical Journal , keywords =. doi:10.1088/0004-637X/778/1/56 , archivePrefix =. 1310.1527 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/778/1/56

  22. [22]

    High-Resolution Spectroscopy of Extremely Metal-Poor Stars in the Least Evolved Galaxies: Ursa Major II and Coma Berenices

    High-Resolution Spectroscopy of Extremely Metal-Poor Stars in the Least Evolved Galaxies: Ursa Major II and Coma Berenices. The Astrophysical Journal , keywords =. doi:10.1088/0004-637X/708/1/560 , archivePrefix =. 0902.2395 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/708/1/560

  23. [23]

    Segue 1: An Unevolved Fossil Galaxy from the Early Universe

    Segue 1: An Unevolved Fossil Galaxy from the Early Universe. The Astrophysical Journal , keywords =. doi:10.1088/0004-637X/786/1/74 , archivePrefix =. 1403.6116 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/786/1/74

  24. [24]

    Abundances for metal-poor stars with accurate parallaxes. II. alpha -elements in the halo. Astronomy & Astrophysics , keywords =. doi:10.1051/0004-6361:20030754 , archivePrefix =. astro-ph/0305358 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20030754

  25. [25]

    Silver and palladium help unveil the nature of a second r-process

    Silver and palladium help unveil the nature of a second r-process. Astronomy & Astrophysics , keywords =. doi:10.1051/0004-6361/201118643 , archivePrefix =. 1205.4744 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201118643

  26. [26]

    Ages and heavy element abundances from very metal-poor stars in the Sagittarius dwarf galaxy

    Ages and Heavy Element Abundances from Very Metal-poor Stars in the Sagittarius Dwarf Galaxy. The Astrophysical Journal , keywords =. doi:10.3847/1538-4357/aa978f , archivePrefix =. 1711.02101 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aa978f

  27. [27]

    VLT/FLAMES high-resolution chemical abundances in Sculptor: a textbook dwarf spheroidal galaxy

    VLT/FLAMES high-resolution chemical abundances in Sculptor: a textbook dwarf spheroidal galaxy. Astronomy & Astrophysics , keywords =. doi:10.1051/0004-6361/201833950 , archivePrefix =. 1812.01486 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201833950

  28. [28]

    Chemical Abundances of the Milky Way Thick Disk and Stellar Halo. I. Implications of [ /Fe] for Star Formation Histories in Their Progenitors. The Astrophysical Journal , keywords =. doi:10.1088/0004-637X/753/1/64 , archivePrefix =. 1205.2406 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/753/1/64

  29. [29]

    Chemical Abundances of the Milky Way Thick Disk and Stellar Halo. II. Sodium, Iron-peak, and Neutron-capture Elements. The Astrophysical Journal , keywords =. doi:10.1088/0004-637X/771/1/67 , archivePrefix =. 1306.0954 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/771/1/67

  30. [30]

    High-Resolution Spectroscopic Study of Extremely Metal-Poor Star Candidates from the SkyMapper Survey

    High-Resolution Spectroscopic Study of Extremely Metal-Poor Star Candidates from the SkyMapper Survey. The Astrophysical Journal , keywords =. doi:10.1088/0004-637X/807/2/171 , archivePrefix =. 1504.03344 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/807/2/171

  31. [31]

    Detailed Abundances for 28 Metal-poor Stars: Stellar Relics in the Milky Way

    Detailed Abundances for 28 Metal-poor Stars: Stellar Relics in the Milky Way. The Astrophysical Journal , keywords =. doi:10.1086/588811 , archivePrefix =. 0804.1370 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/588811

  32. [32]

    Astronomical Journal , keywords =

    Phosphorus Abundances in the Hyades and Galactic Disk. Astronomical Journal , keywords =. doi:10.3847/1538-3881/ab4a1a , archivePrefix =. 1910.00044 , primaryClass =

    work page doi:10.3847/1538-3881/ab4a1a 1910

  33. [33]

    Sulphur and zinc abundances in Galactic halo stars revisited

    Sulphur and zinc abundances in Galactic halo stars revisited. Astronomy & Astrophysics , keywords =. doi:10.1051/0004-6361:20077344 , archivePrefix =. astro-ph/0702689 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20077344

  34. [34]

    Carbon and oxygen abundances in stellar populations

    Carbon and oxygen abundances in stellar populations. Astronomy & Astrophysics , keywords =. doi:10.1051/0004-6361/201424184 , archivePrefix =. 1406.5218 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201424184

  35. [35]

    Astronomical Journal , keywords =

    Carbon Abundances for Red Giants in the Draco Dwarf Spheroidal Galaxy. Astronomical Journal , keywords =. doi:10.1088/0004-6256/145/5/123 , adsurl =

    work page doi:10.1088/0004-6256/145/5/123

  36. [36]

    First stars VI - Abundances of C, N, O, Li, and mixing in extremely metal-poor giants. Galactic evolution of the light elements

    First stars VI - Abundances of C, N, O, Li, and mixing in extremely metal-poor giants. Galactic evolution of the light elements. Astronomy & Astrophysics , keywords =. doi:10.1051/0004-6361:20041274 , archivePrefix =. astro-ph/0409536 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20041274

  37. [37]

    Oxygen Abundances in Nearby FGK Stars and the Galactic Chemical Evolution of the Local Disk and Halo

    Oxygen Abundances in Nearby FGK Stars and the Galactic Chemical Evolution of the Local Disk and Halo. The Astrophysical Journal , keywords =. doi:10.1088/0004-637X/764/1/78 , archivePrefix =. 1301.1582 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/764/1/78

  38. [38]

    The Astrophysical Journal , keywords =

    Fluorine in the Solar Neighborhood: The Need for Several Cosmic Sources. The Astrophysical Journal , keywords =. doi:10.3847/1538-4357/ab7eb1 , archivePrefix =. 2003.04656 , primaryClass =

    work page doi:10.3847/1538-4357/ab7eb1 2003

  39. [39]

    Nucleosynthesis and the Inhomogeneous Chemical Evolution of the Carina Dwarf Galaxy

    Nucleosynthesis and the Inhomogeneous Chemical Evolution of the Carina Dwarf Galaxy. The Astrophysical Journal , keywords =. doi:10.1088/0004-637X/751/2/102 , archivePrefix =. 1204.0787 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/751/2/102

  40. [40]

    and Roederer, Ian U

    Sneden, Christopher and Boesgaard, Ann Merchant and Cowan, John J. and Roederer, Ian U. and Den Hartog, Elizabeth A. and Lawler, James E. , title =. The Astrophysical Journal , year =

  41. [41]

    Annual Review of Astronomy and Astrophysics , volume=

    Star formation in galaxies along the Hubble sequence , author=. Annual Review of Astronomy and Astrophysics , volume=. 1998 , publisher=

    1998

  42. [42]

    Astronomy & Astrophysics , volume=

    Effects of the radial flows on the chemical evolution of the Milky Way disk , author=. Astronomy & Astrophysics , volume=. 2011 , publisher=

    2011

  43. [43]

    Astronomy & Astrophysics , volume=

    The G-dwarf distribution in star-forming galaxies: A tug of war between infall and outflow , author=. Astronomy & Astrophysics , volume=. 2021 , publisher=

    2021

  44. [44]

    The high-redshift formation scenario , author=

    Photochemical evolution of elliptical galaxies--I. The high-redshift formation scenario , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2004 , publisher=

    2004

  45. [45]

    The Astronomy and Astrophysics Review , volume=

    Modelling the chemical evolution of the Milky Way , author=. The Astronomy and Astrophysics Review , volume=. 2021 , publisher=

    2021

  46. [46]

    The solar vicinity , author=

    Chemodynamical evolution of the Milky Way disk-I. The solar vicinity , author=. Astronomy & Astrophysics , volume=. 2013 , publisher=

    2013

  47. [47]

    and Lugaro, Maria

    Kobayashi, Chiaki and Karakas, Amanda I. and Lugaro, Maria. The Origin of Elements from Carbon to Uranium. Astrophys. J. 2020. doi:10.3847/1538-4357/abae65. arXiv:2008.04660

    work page doi:10.3847/1538-4357/abae65 2020

  48. [48]

    The Astrophysical Journal Letters , volume=

    Evolution of fluorine in the Galaxy with the -process , author=. The Astrophysical Journal Letters , volume=. 2011 , publisher=

    2011

  49. [49]

    The Astrophysical Journal , volume=

    Iron-group abundances in the metal-poor main-sequence turnoff star HD 84937 , author=. The Astrophysical Journal , volume=. 2016 , publisher=

    2016

  50. [50]

    Presupernova evolution and explosive nucleosynthesis of rotating massive stars in the metallicity range -3 <=[Fe/H]<= 0

    Limongi, Marco and Chieffi, Alessandro. Presupernova Evolution and Explosive Nucleosynthesis of Rotating Massive Stars in the Metallicity Range - 3 [Fe/H] 0. Astrophys. J. Suppl. 2018. doi:10.3847/1538-4365/aacb24. arXiv:1805.09640

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4365/aacb24 2018

  51. [51]

    , author=

    The luminosity function and stellar evolution. , author=. Astrophysical Journal, vol. 121, p. 161 , volume=

  52. [52]

    Single stars

    On the variation of the initial mass function. MNRAS , keywords =. doi:10.1046/j.1365-8711.2001.04022.x , archivePrefix =. astro-ph/0009005 , primaryClass =

    work page doi:10.1046/j.1365-8711.2001.04022.x 2001

  53. [53]

    Encyclopedia of Astrophysics , year = 2026, volume =

    The initial mass function of stars. Encyclopedia of Astrophysics , year = 2026, volume =. doi:10.1016/B978-0-443-21439-4.00035-3 , adsurl =

    work page doi:10.1016/b978-0-443-21439-4.00035-3 2026

  54. [54]

    The origin and evolution of the odd-Z iron-peak elements Sc, V, Mn, and Co in the Milky Way stellar disk

    The origin and evolution of the odd-Z iron-peak elements Sc, V, Mn, and Co in the Milky Way stellar disk. Astronomy & Astrophysics , keywords =. doi:10.1051/0004-6361/201425327 , archivePrefix =. 1502.01152 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201425327

  55. [55]

    alpha-, r-, and s-process element trends in the Galactic thin and thick disks

    -, r-, and s-process element trends in the Galactic thin and thick disks. Astronomy & Astrophysics , keywords =. doi:10.1051/0004-6361:20040332 , archivePrefix =. astro-ph/0412132 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20040332

  56. [56]

    Stellar Abundances in the Solar Neighborhood: The Hypatia Catalog

    Stellar Abundances in the Solar Neighborhood: The Hypatia Catalog. Astronomical Journal , keywords =. doi:10.1088/0004-6256/148/3/54 , archivePrefix =. 1405.6719 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-6256/148/3/54

  57. [57]

    , keywords =

    Stellar migration and chemical enrichment in the milky way disc: a hybrid model. , keywords =. doi:10.1093/mnras/stab2718 , archivePrefix =. 2103.09838 , primaryClass =

    work page doi:10.1093/mnras/stab2718

  58. [58]

    , keywords =

    Assessing stellar yields in Galaxy chemical evolution: Observational stellar abundance patterns. , keywords =. doi:10.1093/mnras/stad1013 , archivePrefix =. 2304.00208 , primaryClass =

    work page doi:10.1093/mnras/stad1013

  59. [59]

    , keywords =

    Production of ^ 44 Ti and Iron-group Nuclei in the Ejecta of 3D Neutrino-driven Supernovae. , keywords =. doi:10.3847/2041-8213/ad045b , archivePrefix =. 2308.09659 , primaryClass =

    work page doi:10.3847/2041-8213/ad045b 2041

  60. [60]

    Trends in Ti44 and Ni56 from Core-Collapse Supernovae

    Trends in ^ 44 Ti and ^ 56 Ni from Core-collapse Supernovae. , keywords =. doi:10.1088/0067-0049/191/1/66 , archivePrefix =. 1009.3175 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0067-0049/191/1/66

  61. [61]

    , keywords =

    Reaction Rate Sensitivity of the Production of -Ray Emitting Isotopes in Core-collapse Supernovae. , keywords =. doi:10.3847/1538-4357/abafb5 , adsurl =

    work page doi:10.3847/1538-4357/abafb5

  62. [62]

    , keywords =

    Metallicity-dependent nucleosynthetic yields of Type Ia supernovae originating from double detonations of sub-M _ Ch white dwarfs. , keywords =. doi:10.1051/0004-6361/202140881 , archivePrefix =. 2103.14050 , primaryClass =

    work page doi:10.1051/0004-6361/202140881

  63. [63]

    , keywords =

    Stellar initial mass function varies with metallicity and time. , keywords =. doi:10.1038/s41586-022-05488-1 , archivePrefix =. 2301.07029 , primaryClass =

    work page doi:10.1038/s41586-022-05488-1

  64. [64]

    2003, MNRAS, 341, 1179, doi: 10.1046/j.1365-8711.2003.06473.x

    The chemical compositions of Galactic disc F and G dwarfs. Monthly Notices of the Royal Astronomical Society , keywords =. doi:10.1046/j.1365-8711.2003.06305.x , archivePrefix =. astro-ph/0211551 , primaryClass =

    work page doi:10.1046/j.1365-8711.2003.06305.x 2003

  65. [65]

    Constraining cosmic scatter in the Galactic halo through a differential analysis of metal-poor stars

    Constraining cosmic scatter in the Galactic halo through a differential analysis of metal-poor stars. Astronomy & Astrophysics , keywords =. doi:10.1051/0004-6361/201730750 , archivePrefix =. 1709.03750 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201730750

  66. [66]

    The Most Metal-poor Stars. II. Chemical Abundances of 190 Metal-poor Stars Including 10 New Stars with [Fe/H] <= -3.5. The Astrophysical Journal , keywords =. doi:10.1088/0004-637X/762/1/26 , archivePrefix =. 1208.3003 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/762/1/26

  67. [67]

    Core-Collapse Supernovae from 9 to 120 Solar Masses Based on Neutrino-powered Explosions

    Core-collapse Supernovae from 9 to 120 Solar Masses Based on Neutrino-powered Explosions. , keywords =. doi:10.3847/0004-637X/821/1/38 , archivePrefix =. 1510.04643 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/0004-637x/821/1/38

  68. [68]

    Nucleosynthesis yields of core-collapse supernovae and hypernovae, and galactic chemical evolution , journal =

    Ken'ichi Nomoto and Nozomu Tominaga and Hideyuki Umeda and Chiaki Kobayashi and Keiichi Maeda , keywords =. Nucleosynthesis yields of core-collapse supernovae and hypernovae, and galactic chemical evolution , journal =. 2006 , note =. doi:https://doi.org/10.1016/j.nuclphysa.2006.05.008 , url =

    work page doi:10.1016/j.nuclphysa.2006.05.008 2006

  69. [69]

    Annual Review of Astronomy and Astrophysics , year =

    Ken'ichi Nomoto and Chiaki Kobayashi and Nobuya Tominaga , title =. Annual Review of Astronomy and Astrophysics , year =

  70. [70]

    Galactic chemical enrichment with new metallicity dependent yields

    Portinari, L. and Chiosi, C. and Bressan, A. Galactic chemical enrichment with new metallicity dependent yields. Astron. Astrophys. 1998. arXiv:astro-ph/9711337

    work page internal anchor Pith review Pith/arXiv arXiv 1998

  71. [71]

    GalCEM. I. An Open-source Detailed Isotopic Chemical Evolution Code. , keywords =. doi:10.3847/1538-4365/aca7c7 , archivePrefix =. 2301.02257 , primaryClass =

    work page doi:10.3847/1538-4365/aca7c7

  72. [72]

    , keywords =

    Relative roles of type I and II supernovae in the chemical enrichment of the interstellar gas. , keywords =

  73. [73]

    doi:10.1007/978-3-642-22491-1 , adsurl =

    Chemical Evolution of Galaxies. doi:10.1007/978-3-642-22491-1 , adsurl =

    work page doi:10.1007/978-3-642-22491-1

  74. [74]

    Chemical evolution with rotating massive star yields: I. The solar neighbourhood and the s-process elements

    Chemical evolution with rotating massive star yields - I. The solar neighbourhood and the s-process elements. , keywords =. doi:10.1093/mnras/sty316 , archivePrefix =. 1802.02824 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty316

  75. [75]

    Evolution, nucleosynthesis and yields of AGB stars at different metallicities (III): intermediate mass models, revised low mass models and the ph-FRUITY interface

    Cristallo, S. and Straniero, O. and Piersanti, L. and Gobrecht, D. Evolution, nucleosynthesis and yields of AGB stars at different metallicities (III): intermediate mass models, revised low mass models and the ph-FRUITY interface. Astrophys. J. Suppl. 2015. doi:10.1088/0067-0049/219/2/40. arXiv:1507.07338

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0067-0049/219/2/40 2015

  76. [76]

    Nucleosynthesis in Chandrasekhar Mass Models for Type Ia Supernovae and Constraints on Progenitor Systems and Burning-Front Propagation

    Iwamoto, Koichi and Brachwitz, Franziska and Nomoto, Ken'ichi and Kishimoto, Nobuhiro and Umeda, Hideyuki and Hix, W. Raphael and Thielemann, Friedrich-K. Nucleosynthesis in Chandrasekhar mass models for type Ia supernovae and constraints on progenitor systems and burning-front propagation. Astrophys. J. Suppl. 2000. doi:10.1086/313278. arXiv:astro-ph/0002337

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/313278 2000

  77. [77]

    Unusual [Sc/Fe], [V/Fe], and [Y/Fe] Abundance Ratios in the Galactic Center: Evidence for a Top-heavy Initial Mass Function?

    Do, Tuan and Kerzendorf, Wolfgang and Dehnen, Walter and Ghez, Andrea and Lu, Jessica and Sch \"o del, Rainer and Morris, Mark. Unusual [Sc/Fe], [V/Fe], and [Y/Fe] Abundance Ratios in the Galactic Center: Evidence for a Top-heavy Initial Mass Function?. The Astrophysical Journal Letters. 2018. doi:10.3847/2041-8213/aaaec3

    work page doi:10.3847/2041-8213/aaaec3 2018

  78. [78]

    Astronomy & Astrophysics , year =

    Meynet, Georges and Maeder, Andre , title =. Astronomy & Astrophysics , year =

  79. [79]

    Monthly Notices of the Royal Astronomical Society , year =

    Chiappini, Cristina and Romano, Donatella and Matteucci, Francesca , title =. Monthly Notices of the Royal Astronomical Society , year =

  80. [80]

    Astronomy & Astrophysics , year =

    Chiappini, Cristina and Matteucci, Francesca and Meynet, Georges , title =. Astronomy & Astrophysics , year =

Showing first 80 references.