Pith Number

pith:U6PQ7K6I

pith:2026:U6PQ7K6I6LW7LU7KT2WKN6ZUJJ

not attested not anchored not stored refs resolved

Observational Signatures and Constraints on the Intermediate Neutron-Capture Process. The Case of the CEMP star TYC 6044-714-1 (RAVE J094921.8-161722)

Deysi Cornejo Espinoza, Diego Vescovi, Laura Magrini, Luciano Piersanti, Martina Baratella, Riano E. Giribaldi, Sergio Cristallo, Sofia Randich, Valentina D'Orazi

High-precision abundances in CEMP star TYC 6044-714-1 favor the s+r model over i-process variants for the heavy-element pattern and Ba isotopic ratios.

arxiv:2605.11074 v2 · 2026-05-11 · astro-ph.SR

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\usepackage{pith}
\pithnumber{U6PQ7K6I6LW7LU7KT2WKN6ZUJJ}

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Record completeness

1 Bitcoin timestamp

2 Internet Archive

3 Author claim open · sign in to claim

4 Citations open

5 Replications open

✓ Portable graph bundle live · download bundle · merged state

The bundle contains the canonical record plus signed events. A mirror can host it anywhere and recompute the same current state with the deterministic merge algorithm.

Claims

C1strongest claim

The s+r model provides the best overall reproduction of the observed heavy-element abundance pattern and Ba isotopic ratios, yielding excellent agreement across all three s-process peaks. While i+s+r models with increasing overshooting efficiency improve the fit for specific elements, they do not consistently reproduce the full abundance pattern.

C2weakest assumption

The assumption that the latest AGB nucleosynthesis models, including their treatment of overshooting and neutron-capture rates, provide a sufficiently complete and accurate representation of possible i-process conditions in low-mass metal-poor stars without missing key physical ingredients.

C3one line summary

High-precision abundances and Ba isotopic ratios in TYC 6044-714-1 favor an s+r nucleosynthesis scenario over i-process models, which require implausible conditions and mismatch isotopic data.

References

292 extracted · 292 resolved · 134 Pith anchors

[1] Carbon-Enhanced Metal-Poor Star Frequencies in the Galaxy: Corrections for the Effect of Evolutionary Status on Carbon Abundances · doi:10.1088/0004-637x/797/1/21

[2] Silver and palladium help unveil the nature of a second r-process · doi:10.1051/0004-6361/201118643

[3] J., & Gallino, R.\ 2008, , 46, 241 2008 · doi:10.1146/annurev.astro.46.060407.145207

[4] Mixing along the red giant branch in metal-poor field stars. , keywords =

[5] The puzzle of the CNO isotope ratios in AGB carbon stars · doi:10.1051/0004-6361/201629969

Receipt and verification

First computed	2026-05-20T00:01:43.885766Z
Builder	pith-number-builder-2026-05-17-v1
Signature	Pith Ed25519 (`pith-v1-2026-05`) · public key
Schema	pith-number/v1.0

Canonical hash

a79f0fabc8f2edf5d3ea9eaca6fb344a4b9fc3ffdb46005d412936245e7d752a

Aliases

arxiv: 2605.11074 · arxiv_version: 2605.11074v2 · doi: 10.48550/arxiv.2605.11074 · pith_short_12: U6PQ7K6I6LW7 · pith_short_16: U6PQ7K6I6LW7LU7K · pith_short_8: U6PQ7K6I

Agent API

Resolver JSON Graph JSON Events JSON Schema Signing key

Verify this Pith Number yourself

curl -sH 'Accept: application/ld+json' https://pith.science/pith/U6PQ7K6I6LW7LU7KT2WKN6ZUJJ \
  | jq -c '.canonical_record' \
  | python3 -c "import sys,json,hashlib; b=json.dumps(json.loads(sys.stdin.read()), sort_keys=True, separators=(',',':'), ensure_ascii=False).encode(); print(hashlib.sha256(b).hexdigest())"
# expect: a79f0fabc8f2edf5d3ea9eaca6fb344a4b9fc3ffdb46005d412936245e7d752a

Canonical record JSON

{
  "metadata": {
    "abstract_canon_sha256": "4038c2580e7df729675869cc93f537e7168871cce956927027aa1c5ba44b75ed",
    "cross_cats_sorted": [],
    "license": "http://creativecommons.org/licenses/by/4.0/",
    "primary_cat": "astro-ph.SR",
    "submitted_at": "2026-05-11T18:00:02Z",
    "title_canon_sha256": "17bf05aebcea6c53372cb33bf4d59405ee760ada417ec8767a2d884902836cd3"
  },
  "schema_version": "1.0",
  "source": {
    "id": "2605.11074",
    "kind": "arxiv",
    "version": 2
  }
}