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Uncertainties in the production of p nuclei in massive stars obtained from Monte Carlo variations

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Uncertainties in the production of p nuclei in massive stars obtained from Monte Carlo variations. / Rauscher, T.; Nishimura, N.; Hirschi, R.; Cescutti, G.; Murphy, A. St J.; Heger, A.

In: Monthly Notices of the Royal Astronomical Society, Vol. 463, No. 4, 21.12.2016, p. 4153-4166.

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Rauscher, T. ; Nishimura, N. ; Hirschi, R. ; Cescutti, G. ; Murphy, A. St J. ; Heger, A. / Uncertainties in the production of p nuclei in massive stars obtained from Monte Carlo variations. In: Monthly Notices of the Royal Astronomical Society. 2016 ; Vol. 463, No. 4. pp. 4153-4166.

Bibtex

@article{e5dd309cd1fe40e49b624e74c21b8725,
title = "Uncertainties in the production of p nuclei in massive stars obtained from Monte Carlo variations",
abstract = "Nuclear uncertainties in the production of $p$ nuclei in massive stars have been quantified in a Monte Carlo procedure. Bespoke temperature-dependent uncertainties were assigned to different types of reactions involving nuclei from Fe to Bi. Their simultaneous impact was studied in postprocessing explosive trajectories for three different stellar models. It was found that the grid of mass zones in the model of a 25 $M_\odot$ star, which is widely used for investigations of $p$ nucleosynthesis, is too crude to properly resolve the detailed temperature changes required for describing the production of $p$ nuclei. Using models with finer grids for 15 $M_\odot$ and 25 $M_\odot$ stars with initial solar metallicity, it was found that most of the production uncertainties introduced by nuclear reaction uncertainties are smaller than a factor of two. Since a large number of rates were varied at the same time in the Monte Carlo procedure, possible cancellation effects of several uncertainties could be taken into account. Key rates were identified for each $p$ nucleus, which provide the dominant contribution to the production uncertainty. These key rates were found by examining correlations between rate variations and resulting abundance changes. This method is superior to studying flow patterns, especially when the flows are complex, and to individual, sequential variation of a few rates.",
keywords = "astro-ph.HE, astro-ph.SR, nucl-ex, nucl-th",
author = "T. Rauscher and N. Nishimura and R. Hirschi and G. Cescutti and Murphy, {A. St J.} and A. Heger",
note = "T. Rauscher, N. Nishimura, R. Hirschi, G. Cescutti, A. St. J. Murphy and A. Heger, {\textquoteleft}Uncertainties in the production of p nuclei in massive stars obtained from Monte Carlo variations{\textquoteright}, MNRAS Vol 463( 4 ): 4153-4166, first published online on 8 September 2016, the version of record is available online via doi:10.1093/mnras/stw2266 {\textcopyright} 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. ",
year = "2016",
month = dec,
day = "21",
doi = "10.1093/mnras/stw2266",
language = "English",
volume = "463",
pages = "4153--4166",
journal = "Monthly Notices of the Royal Astronomical Society",
issn = "0035-8711",
publisher = "Oxford University Press",
number = "4",

}

RIS

TY - JOUR

T1 - Uncertainties in the production of p nuclei in massive stars obtained from Monte Carlo variations

AU - Rauscher, T.

AU - Nishimura, N.

AU - Hirschi, R.

AU - Cescutti, G.

AU - Murphy, A. St J.

AU - Heger, A.

N1 - T. Rauscher, N. Nishimura, R. Hirschi, G. Cescutti, A. St. J. Murphy and A. Heger, ‘Uncertainties in the production of p nuclei in massive stars obtained from Monte Carlo variations’, MNRAS Vol 463( 4 ): 4153-4166, first published online on 8 September 2016, the version of record is available online via doi:10.1093/mnras/stw2266 © 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.

PY - 2016/12/21

Y1 - 2016/12/21

N2 - Nuclear uncertainties in the production of $p$ nuclei in massive stars have been quantified in a Monte Carlo procedure. Bespoke temperature-dependent uncertainties were assigned to different types of reactions involving nuclei from Fe to Bi. Their simultaneous impact was studied in postprocessing explosive trajectories for three different stellar models. It was found that the grid of mass zones in the model of a 25 $M_\odot$ star, which is widely used for investigations of $p$ nucleosynthesis, is too crude to properly resolve the detailed temperature changes required for describing the production of $p$ nuclei. Using models with finer grids for 15 $M_\odot$ and 25 $M_\odot$ stars with initial solar metallicity, it was found that most of the production uncertainties introduced by nuclear reaction uncertainties are smaller than a factor of two. Since a large number of rates were varied at the same time in the Monte Carlo procedure, possible cancellation effects of several uncertainties could be taken into account. Key rates were identified for each $p$ nucleus, which provide the dominant contribution to the production uncertainty. These key rates were found by examining correlations between rate variations and resulting abundance changes. This method is superior to studying flow patterns, especially when the flows are complex, and to individual, sequential variation of a few rates.

AB - Nuclear uncertainties in the production of $p$ nuclei in massive stars have been quantified in a Monte Carlo procedure. Bespoke temperature-dependent uncertainties were assigned to different types of reactions involving nuclei from Fe to Bi. Their simultaneous impact was studied in postprocessing explosive trajectories for three different stellar models. It was found that the grid of mass zones in the model of a 25 $M_\odot$ star, which is widely used for investigations of $p$ nucleosynthesis, is too crude to properly resolve the detailed temperature changes required for describing the production of $p$ nuclei. Using models with finer grids for 15 $M_\odot$ and 25 $M_\odot$ stars with initial solar metallicity, it was found that most of the production uncertainties introduced by nuclear reaction uncertainties are smaller than a factor of two. Since a large number of rates were varied at the same time in the Monte Carlo procedure, possible cancellation effects of several uncertainties could be taken into account. Key rates were identified for each $p$ nucleus, which provide the dominant contribution to the production uncertainty. These key rates were found by examining correlations between rate variations and resulting abundance changes. This method is superior to studying flow patterns, especially when the flows are complex, and to individual, sequential variation of a few rates.

KW - astro-ph.HE

KW - astro-ph.SR

KW - nucl-ex

KW - nucl-th

U2 - 10.1093/mnras/stw2266

DO - 10.1093/mnras/stw2266

M3 - Article

VL - 463

SP - 4153

EP - 4166

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

IS - 4

ER -