Pith Number

pith:JP6VBWHM

pith:2026:JP6VBWHMLUOEQOPC53ERE3HMFO

not attested not anchored not stored refs resolved

Dynamical response of twin stars to perturbations

Luciano Rezzolla, Ritam Mallick, Shamim Haque

Twin stars on the two branches have different critical perturbation strengths that determine which configuration is dynamically favored.

arxiv:2602.02654 v2 · 2026-02-02 · gr-qc · astro-ph.HE · nucl-th

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Record completeness

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2 Internet Archive

3 Author claim open · sign in to claim

4 Citations open

5 Replications open

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Claims

C1strongest claim

Because the critical values are different for stars with the same rest-mass but sitting on either branch, it is possible to define as favoured the part of the branch that has the largest critical perturbation, thus correcting the common wisdom that stellar models on the twin branch are the favoured ones. Interestingly, we show that the binding energies on the two branches can be used to deduce without simulations which of the stellar configurations is more likely to be found in nature.

C2weakest assumption

The assumption that the chosen equations of state produce stable twin branches and that the numerical hydrodynamics accurately captures the nonlinear migration threshold without resolution or artificial viscosity artifacts.

C3one line summary

Twin-star configurations on the hadronic branch are dynamically favored over hybrid twins because they tolerate stronger perturbations before migrating, with binding energies serving as a proxy for this preference.

References

75 extracted · 75 resolved · 6 Pith anchors

[1] Resolution dependence We first discuss the robustness of our conclusion and present evidence that the resolution employed is adequate to measure the critical perturbation velocity inducing the mi- gra

[2] To validate this dependence, we have considered the migration dynamics using velocity perturbation profiles with different profiles

[3] Comparison of stable evolution with perturbative results As anticipated in the main text, the stars on TB and HB are linearly stable and hence will undergo (damped) oscillations when exposed to linear

[4] III D, we have also considered the evo- lution of other classes of twin stars

[5] L. Rezzolla, P. Pizzochero, D. I. Jones, N. Rea, and I. Vida ˜na, eds.,The Physics and Astrophysics of Neutron Stars, Astro- physics and Space Science Library, V ol. 457 (Springer, 2018) 2018

Formal links

2 machine-checked theorem links

Receipt and verification

First computed	2026-06-01T02:03:34.082586Z
Builder	pith-number-builder-2026-05-17-v1
Signature	Pith Ed25519 (`pith-v1-2026-05`) · public key
Schema	pith-number/v1.0

Canonical hash

4bfd50d8ec5d1c4839e2eec9126cec2b98f69eb6f5d206dbc2a4102817a93ea2

Aliases

arxiv: 2602.02654 · arxiv_version: 2602.02654v2 · doi: 10.48550/arxiv.2602.02654 · pith_short_12: JP6VBWHMLUOE · pith_short_16: JP6VBWHMLUOEQOPC · pith_short_8: JP6VBWHM

Agent API

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Verify this Pith Number yourself

curl -sH 'Accept: application/ld+json' https://pith.science/pith/JP6VBWHMLUOEQOPC53ERE3HMFO \
  | 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: 4bfd50d8ec5d1c4839e2eec9126cec2b98f69eb6f5d206dbc2a4102817a93ea2

Canonical record JSON

{
  "metadata": {
    "abstract_canon_sha256": "caa24b388e6ae0519bf9398b4c3ae834b987c1b0a6622c9099bd28b52b6144b0",
    "cross_cats_sorted": [
      "astro-ph.HE",
      "nucl-th"
    ],
    "license": "http://creativecommons.org/licenses/by/4.0/",
    "primary_cat": "gr-qc",
    "submitted_at": "2026-02-02T19:00:01Z",
    "title_canon_sha256": "ff3cb23de007054e820967fb93619c45e9c3ba99f4745fa60c32299595a6e5b4"
  },
  "schema_version": "1.0",
  "source": {
    "id": "2602.02654",
    "kind": "arxiv",
    "version": 2
  }
}