# Nuclear Partition Functions at Temperatures Exceeding 10 10 K

@article{Rauscher2003NuclearPF, title={Nuclear Partition Functions at Temperatures Exceeding 10 10 K}, author={Thomas Rauscher}, journal={Astrophysical Journal Supplement Series}, year={2003}, volume={147}, pages={403-408} }

Nuclear partition functions were calculated for a grid of temperatures from 1.2 × 1010 to 2.75 × 1011 K (1 MeV ≤ kT ≤ 24 MeV) within a Fermi-gas approach, including all nuclides from the proton-dripline to the neutron-dripline with proton number 9 ≤ Z ≤ 85. The calculation is based on a nuclear level density description published elsewhere, thus extending the previous tables of partition functions beyond 1010 K. Additional high-temperature corrections had to be applied.

## 24 Citations

Temperature-dependent nuclear partition functions and abundances in the stellar interior

- Physics
- 2016

We calculate the temperature-dependent nuclear partition functions (TDNPFs) and nuclear abundances for 728 nuclei, assuming nuclear statistical equilibrium (NSE). The theories of stellar evolution…

Large-scale prediction of the parity distribution in the nuclear level density and application to astrophysical reaction rates

- Physics
- 2007

A generalized method to calculate the excitation-energy dependent parity ratio in the nuclear level density is presented, using the assumption of Poisson distributed independent quasi particles…

Electron fraction constraints based on Nuclear Statistical Equilibrium with beta equilibrium

- Physics
- 2010

The electron-to-nucleon ratio or electron fraction is a key parameter in many astrophysical studies. Its value is determined by weakinteraction rates that are based on theoretical calculations…

Sensitivity of nuclear statistical equilibrium to nuclear uncertainties during stellar core collapse

- PhysicsPhysical Review C
- 2018

I have systematically investigated the equations of state (EOSs) in nuclear statistical equilibrium under thermodynamic conditions relevant for core collapse of massive stars by varying the bulk…

Nuclear Statistical Equilibrium equation of state for core collapse

- PhysicsNuclear Physics A
- 2019

Abstract Extensive calculations of properties of supernova matter are presented, using the extended Nuclear Statistical Equilibrium model of Ref. [1] based on a statistical distribution of…

Nuclear statistical equilibrium at core-collapse supernova

- Physics
- 2007

A new improved nuclear partition function is employed to calculate the nuclear statistical equilibrium (NSE) in core-collapse supernova environment. The results show that the change of nucleus…

Allowed and unique first-forbidden stellar electron emission rates of neutron-rich copper isotopes

- Physics
- 2017

The allowed charge-changing transitions are the most common weak interaction processes of spin-isospin form that play a crucial role in several nuclear/astrophysical processes. The first-forbidden…

Improved estimate of electron capture rates on nuclei during stellar core collapse

- Physics
- 2010

Abstract Electron captures on nuclei play an important role in the dynamics of the collapsing core of a massive star that leads to a supernova explosion. Recent calculations of these capture rates…

A statistical model for a complete supernova equation of state

- Physics
- 2010

Abstract A statistical model for the equation of state and the composition of supernova matter is presented. It consists of an ensemble of nuclei and interacting nucleons in nuclear statistical…

Sensitivity studies on the excited states of nuclei in beta decays in the r-process of neutron star mergers

- Physics
- 2020

Sensitivity studies conducted in this paper aim to examine the influence of uncertainties in beta decay rates on simulations of rapid neutron capture (r-process) nucleosynthesis. However, previous…

## References

SHOWING 1-8 OF 8 REFERENCES

Nuclear partition functions at high temperature

- Physics
- 1979

Nuclear partition functions are calculated in a Fermi-gas approximation which accounts for continuum single-particle orbitals. Numerical results for iron-peak nuclei with kT< or =10 MeV indicate that…

Neutron star matter at high temperatures and densities. I. Bulk properties of nuclear matter

- Physics
- 1978

We perform calculations of the thermodynamic properties of uniform dense matter at finite temperature using the Skyrme nuclear interaction. The calculations are valid for arbitrary proton…

Nuclear level density and the determination of thermonuclear rates for astrophysics

- Physics
- 1997

The prediction of cross sections for nuclei far off stability is crucial in the field of nuclear astrophysics. In recent calculations the nuclear level density{emdash}as an important ingredient to…

Nuclear ground state masses and deformations

- Physics
- 1995

Abstract We tabulate the atomic mass excesses and nuclear ground-state deformations of 8979 nuclei ranging from 16O to A = 339. The calculations are based on the finite-range droplet macroscopic…

Astrophysical reaction rates from statistical model calculations

- Chemistry, Physics
- 2000

Theoretical reaction rates in the temperature range 0.01 x 10(9) less than or equal to T(K) less than or equal to 10.0 x 10(9) are calculated in the statistical model (Hauser-Feshbach formalism) for…

Tables of nuclear cross sections and reaction rates : An addendum to the paper "Astrophysical reaction rates from statistical model calculations"

- Physics, Chemistry
- 2001

In a previous publication (ATOMIC DATA AND NUCLEAR DATA TABLES 75, 1 (2000)), we gave seven-parameter analytical fits to theoretical reaction rates derived from nuclear cross sections calculated in…

Nuclear mass formula with Bogolyubov-enhanced shell-quenching: application to r-process

- Physics
- 1996

The ETFSI mass table, which is based entirely on microscopic forces, has been modified to take account of the strong quenching of shell effects found in HFB calculations on highly neutron-rich…