From Giant Envelopes to Rapidly Contracting Cores in Rotating Population III Stars from $500$ to 1000 M_⊙

Abstract

Population III (Pop III) stars link the chemical enrichment of the early Universe to the formation of the first massive black holes, yet their evolution remains poorly understood at extreme masses. Using GENEC, we evolve rotating zero metallicity models from $500$ to 1000 M_⊙ at v/v_crit=0.1 through core Si burning, and a 1000 M_⊙, v/v_crit=0.4 model evolved through He exhaustion. In the fiducial 1000 M_⊙ model, convection and rotational transport carry freshly synthesized C and O into H burning layers, producing 62.1 M_⊙ of primary N by He exhaustion. Surface mass loss removes 20.2 M_⊙, including 1.8×10⁻³ M_⊙ of N, with log(N/O)=0.68, log(N/C)=1.48, and log(C/O)=−0.80. By the final hydrostatic model, the inner 100 M_⊙ is confined within 0.088 R_⊙ while the photosphere remains several thousand solar radii away. As C, Ne, O, and Si burning accelerate, chemical mixing freezes out and advanced products remain buried beneath the envelope. At core Si exhaustion, the central angular velocity reaches 4×10⁻³ s⁻¹ while the surface rotates at 5.25×10⁻⁸ s⁻¹, a contrast of 7.6×10⁴. Contraction drives this spin up, while inner specific angular momentum changes by less than 1%. The maximum j_eq/j_ISCO is $0.313$, limiting disk formation in our inside out estimate. These models show that Pop~III stars can produce strong primary N signatures and rapidly rotating black hole progenitors while their envelopes determine which products enrich the early Universe.

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BibTeX RIS

BibTeX

@misc{nandal2026from,
  title = {{From Giant Envelopes to Rapidly Contracting Cores in Rotating Population III Stars from $500$ to $1000 \, M_\odot$}},
  author = {Devesh Nandal and John Chisholm and Daniel J. Whalen and Andreas A. C. Sander and Volker Bromm and Peixin Zhu and Lisa J. Kewley},
  howpublished = {arXiv},
  year = {2026},
  month = oct,
  doi = {10.48550/arxiv.2610.17218},
  eprint = {2610.17218},
  archivePrefix = {arXiv},
  url = {https://arxiv.org/abs/2610.17218},
  note = {CC BY 4.0},
}

RIS

TY  - UNPB
TI  - From Giant Envelopes to Rapidly Contracting Cores in Rotating Population III Stars from $500$ to 1000 M_⊙
AU  - Devesh Nandal
AU  - John Chisholm
AU  - Daniel J. Whalen
AU  - Andreas A. C. Sander
AU  - Volker Bromm
AU  - Peixin Zhu
AU  - Lisa J. Kewley
PY  - 2026
DA  - 2026/10/12
PB  - arXiv
DO  - 10.48550/arxiv.2610.17218
UR  - https://arxiv.org/abs/2610.17218
AB  - Population III (Pop III) stars link the chemical enrichment of the early Universe to the formation of the first massive black holes, yet their evolution remains poorly understood at extreme masses. Using GENEC, we evolve rotating zero metallicity models from $500$ to 1000 M_⊙ at v/v_crit=0.1 through core Si burning, and a 1000 M_⊙, v/v_crit=0.4 model evolved through He exhaustion. In the fiducial 1000 M_⊙ model, convection and rotational transport carry freshly synthesized C and O into H burning layers, producing 62.1 M_⊙ of primary N by He exhaustion. Surface mass loss removes 20.2 M_⊙, including 1.8×10^−3 M_⊙ of N, with log(N/O)=0.68, log(N/C)=1.48, and log(C/O)=−0.80. By the final hydrostatic model, the inner 100 M_⊙ is confined within 0.088 R_⊙ while the photosphere remains several thousand solar radii away. As C, Ne, O, and Si burning accelerate, chemical mixing freezes out and advanced products remain buried beneath the envelope. At core Si exhaustion, the central angular velocity reaches 4×10^−3 s^−1 while the surface rotates at 5.25×10^−8 s^−1, a contrast of 7.6×10^4. Contraction drives this spin up, while inner specific angular momentum changes by less than 1%. The maximum j_eq/j_ISCO is $0.313$, limiting disk formation in our inside out estimate. These models show that Pop~III stars can produce strong primary N signatures and rapidly rotating black hole progenitors while their envelopes determine which products enrich the early Universe.
ER  -

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