Neutrino cooling rates due to nickel isotopes for presupernova evolution of massive stars

Nabi, Jameel-Un; Shehzadi, R.; Majid, Muhammad

doi:10.1016/j.newast.2019.03.001

Cited by 2 publications

(2 citation statements)

References 54 publications

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“…Nuclear reaction networks can have a nontrivial effect on the evolution of massive stars (Farmer et al 2016), especially the inclusion of elements like iron and nickel (Nabi et al 2019). Hence, we make use of an extensive grid of isotopes for the nuclear reaction network in our models to closely follow the evolution of massive stars.…”

Section: Physical Ingredientsmentioning

confidence: 99%

A systematic study of super-Eddington layers in the envelopes of massive stars

Agrawal

Stevenson

Szécsi

et al. 2022

A&A

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Context. The proximity to the Eddington luminosity has been attributed as the cause of several observed effects in massive stars. Computationally, if the luminosity carried through radiation exceeds the local Eddington luminosity in the low-density envelopes of massive stars, it can result in numerical difficulties, inhibiting further computation of stellar models. This problem is exacerbated by the fact that very few massive stars are observed beyond the Humphreys-Davidson limit, the same region in the Hertzsprung-Russell diagram where the aforementioned numerical issues relating to the Eddington luminosity occur in stellar models. Aims. One-dimensional stellar evolution codes have to use pragmatic solutions to evolve massive stars through this computationally difficult phase. In this work, we quantify the impact of these solutions on the evolutionary properties of massive stars. Methods. We used the stellar evolution code MESA with commonly used input parameters for massive stellar models to compute the evolution of stars in the initial mass range of 10-110 M ⊙ at one-tenth of solar metallicity. Results. We find that numerical difficulties in stellar models with initial masses greater than or equal to 30 M ⊙ cause these models to fail before the end of core helium burning. Recomputing these models using the same physical inputs but three different pragmatic solutions to treat the numerical instability, we find that the maximum radial expansion achieved by stars can vary by up to 2000 R ⊙ , while the remnant mass of the stars can vary by up to 14 M ⊙ between the sets. These differences can have implications on studies such as binary population synthesis.

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Section: Physical Ingredientsmentioning

confidence: 99%

A systematic study of super-Eddington layers in the envelopes of massive stars

Agrawal

Stevenson

Szécsi

et al. 2022

A&A

View full text Add to dashboard Cite

show abstract

“…Nuclear reaction networks can have a non-trivial effect on the evolution of massive stars (Farmer et al 2016), especially the inclusion of elements like iron and nickel (Nabi et al 2019). Hence, we make use of an extensive grid of isotopes for the nuclear reaction network in our models to closely follow the evolution of massive stars.…”

Section: Stellar Models: the Standard Setmentioning

confidence: 99%

A systematic study of super-Eddington layers in the envelopes of massive stars

Agrawal¹,

Stevenson²,

Szécsi³

et al. 2021

Preprint

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Proximity to the Eddington luminosity has been attributed as the cause of several observed effects in massive stars. Computationally, if the luminosity carried through radiation exceeds the local Eddington luminosity in the low-density envelopes of massive stars, it can result in numerical difficulties, inhibiting further computation of stellar models. This problem is exacerbated by the fact that very few massive stars are observed beyond the Humphreys-Davidson limit, the same region in the Hertzsprung-Russell diagram where the aforementioned numerical issues relating to the Eddington luminosity occur in stellar models. Thus 1D stellar evolution codes have to use pragmatic solutions to evolve massive stars through this computationally difficult phase. In this work, we quantify the impact of these solutions on the evolutionary properties of massive stars. Using the stellar evolution code MESA with commonly used input parameters for massive stellar models, we compute the evolution of stars in the initial mass range of 10-110 M at one-tenth of solar metallicity. We find that numerical difficulties in stellar models with initial masses greater than or equal to 30 M cause these models to fail before the end of core helium burning. Recomputing these models using the same physical inputs but three different numerical methods to treat the numerical instability, we find that the maximum radial expansion achieved by stars can vary by up to 2000 R while the remnant mass of the stars can vary by up to 14 M between the sets. These differences can have implications on studies such as binary population synthesis.

show abstract

Neutrino cooling rates due to nickel isotopes for presupernova evolution of massive stars

Cited by 2 publications

References 54 publications

A systematic study of super-Eddington layers in the envelopes of massive stars

A systematic study of super-Eddington layers in the envelopes of massive stars

A systematic study of super-Eddington layers in the envelopes of massive stars

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