Large nuclear networks in presupernova models

G. Bazán, W David Arnett

Research output: Contribution to journalArticle

4 Citations (Scopus)

Abstract

We outline the role of multidimensional hydrodynamics coupled to large nuclear networks in the case of core silicon burning in massive stars. Using an implementation of the Piecewise Parabolic Method (PPM) of solving the Euler equations for mass, momentum, and total energy, we examine the differences and similarities between a 1-D hydrostatic stellar evolution model and a 2-D hydrodynamical model at two resolutions. We find that 2-D models exhibit significantly less vigorous convection than 1-D hydrostatic models, and that the core compensates for the lack of energy production by increasing temperatures and densities through contraction. Equilibration between the Si-burning and convective timescales appears to occur. Including an 123 isotope network from Ye to 56Ge to the hydrodynamic code leads to similar global behaviors as the 2-D model with the simplified burning algorithm used in the 1-D models. However, significant inhomogeneity in iron peak isotope composition occurs, which could have important consequences to energy losses via electron captures onto G-T resonances and the local energetics which drive convective silicon burning.

Original languageEnglish (US)
JournalNuclear Physics, Section A
Volume621
Issue number1-2
StatePublished - Aug 4 1997

Fingerprint

hydrostatics
isotopes
hydrodynamics
stellar evolution
silicon
massive stars
electron capture
contraction
energy
inhomogeneity
convection
energy dissipation
kinetic energy
iron
temperature

ASJC Scopus subject areas

  • Nuclear and High Energy Physics

Cite this

Large nuclear networks in presupernova models. / Bazán, G.; Arnett, W David.

In: Nuclear Physics, Section A, Vol. 621, No. 1-2, 04.08.1997.

Research output: Contribution to journalArticle

@article{e7100c37dda045adb997d8c7fefa8415,
title = "Large nuclear networks in presupernova models",
abstract = "We outline the role of multidimensional hydrodynamics coupled to large nuclear networks in the case of core silicon burning in massive stars. Using an implementation of the Piecewise Parabolic Method (PPM) of solving the Euler equations for mass, momentum, and total energy, we examine the differences and similarities between a 1-D hydrostatic stellar evolution model and a 2-D hydrodynamical model at two resolutions. We find that 2-D models exhibit significantly less vigorous convection than 1-D hydrostatic models, and that the core compensates for the lack of energy production by increasing temperatures and densities through contraction. Equilibration between the Si-burning and convective timescales appears to occur. Including an 123 isotope network from Ye to 56Ge to the hydrodynamic code leads to similar global behaviors as the 2-D model with the simplified burning algorithm used in the 1-D models. However, significant inhomogeneity in iron peak isotope composition occurs, which could have important consequences to energy losses via electron captures onto G-T resonances and the local energetics which drive convective silicon burning.",
author = "G. Baz{\'a}n and Arnett, {W David}",
year = "1997",
month = "8",
day = "4",
language = "English (US)",
volume = "621",
journal = "Nuclear Physics A",
issn = "0375-9474",
publisher = "Elsevier",
number = "1-2",

}

TY - JOUR

T1 - Large nuclear networks in presupernova models

AU - Bazán, G.

AU - Arnett, W David

PY - 1997/8/4

Y1 - 1997/8/4

N2 - We outline the role of multidimensional hydrodynamics coupled to large nuclear networks in the case of core silicon burning in massive stars. Using an implementation of the Piecewise Parabolic Method (PPM) of solving the Euler equations for mass, momentum, and total energy, we examine the differences and similarities between a 1-D hydrostatic stellar evolution model and a 2-D hydrodynamical model at two resolutions. We find that 2-D models exhibit significantly less vigorous convection than 1-D hydrostatic models, and that the core compensates for the lack of energy production by increasing temperatures and densities through contraction. Equilibration between the Si-burning and convective timescales appears to occur. Including an 123 isotope network from Ye to 56Ge to the hydrodynamic code leads to similar global behaviors as the 2-D model with the simplified burning algorithm used in the 1-D models. However, significant inhomogeneity in iron peak isotope composition occurs, which could have important consequences to energy losses via electron captures onto G-T resonances and the local energetics which drive convective silicon burning.

AB - We outline the role of multidimensional hydrodynamics coupled to large nuclear networks in the case of core silicon burning in massive stars. Using an implementation of the Piecewise Parabolic Method (PPM) of solving the Euler equations for mass, momentum, and total energy, we examine the differences and similarities between a 1-D hydrostatic stellar evolution model and a 2-D hydrodynamical model at two resolutions. We find that 2-D models exhibit significantly less vigorous convection than 1-D hydrostatic models, and that the core compensates for the lack of energy production by increasing temperatures and densities through contraction. Equilibration between the Si-burning and convective timescales appears to occur. Including an 123 isotope network from Ye to 56Ge to the hydrodynamic code leads to similar global behaviors as the 2-D model with the simplified burning algorithm used in the 1-D models. However, significant inhomogeneity in iron peak isotope composition occurs, which could have important consequences to energy losses via electron captures onto G-T resonances and the local energetics which drive convective silicon burning.

UR - http://www.scopus.com/inward/record.url?scp=0031552759&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=0031552759&partnerID=8YFLogxK

M3 - Article

AN - SCOPUS:0031552759

VL - 621

JO - Nuclear Physics A

JF - Nuclear Physics A

SN - 0375-9474

IS - 1-2

ER -