18
M. Herman et al.
to be general and flexible. Each module was designed to perform a well-defined task
and to communicate with other modules through a set of global COMMON blocks.
This assured access to all the resources throughout the code and facilitated the
addition of new features and mechanisms. The third release of the code, EMPIRE-3,
maintains and extends this structure.
The current version, EMPIRE-3.2, is named Malta, after Napoleon’s capture of
the island on the way to Egypt. Although a minor release, it features a number
of significant improvements such as: (1) prompt fission neutron spectra, including
automatic adjustment to experimental data, (2) anisotropic angular distributions
for compound elastic and inelastic excitations, (3) simulation of the EngelbrechtWeidenmüller transformation, and (4) new IO subroutines for the manipulation of
ENDF-6 formatted files.
2 Basic Objectives and Scope
The basic objectives of the EMPIRE code are:
• to provide the state-of-the-art modeling of nuclear reactions for basic science and
data evaluation;
• to ensure reasonably comprehensive coverage of incident particles, targets,
incident energies, and observables;
• To unify (1) reaction models, (2) model parameters, (3) nuclear structure data,
and (4) experimental results;
• to provide a full set of tools for evaluators to enable efficient production of high
quality nuclear data files;
• to be as general, flexible, and easy to use as possible.
The present scope of the code includes:
• A broad range of incident energies (up to 150 MeV) and projectiles (n, p, d, t,
3 He, 4 He, photons, and heavy ions);
• The low-energy range for neutron reactions covered by an interface to the Atlas
of Neutron Resonances [1];
• Default input parameters for targets of mass number A ≥ 20 [2];
• Direct, pre-equilibrium, and statistical model reaction mechanisms—with width
fluctuations and a full gamma cascade;
• Observables: cross sections, angular distributions, spectra (including prompt
fission neutron spectra), energy-angular distributions;
• Outgoing channels: multi-particle emission, γ -emission (including discrete
lines), discrete levels (including isomers), fission, several exclusive channels.
To a large extent, the present scope of the EMPIRE code permits it to fulfill its
objectives. However, it should also be clear that the objectives are an evolving target
that will never be completely met.
M. Herman et al.
to be general and flexible. Each module was designed to perform a well-defined task
and to communicate with other modules through a set of global COMMON blocks.
This assured access to all the resources throughout the code and facilitated the
addition of new features and mechanisms. The third release of the code, EMPIRE-3,
maintains and extends this structure.
The current version, EMPIRE-3.2, is named Malta, after Napoleon’s capture of
the island on the way to Egypt. Although a minor release, it features a number
of significant improvements such as: (1) prompt fission neutron spectra, including
automatic adjustment to experimental data, (2) anisotropic angular distributions
for compound elastic and inelastic excitations, (3) simulation of the EngelbrechtWeidenmüller transformation, and (4) new IO subroutines for the manipulation of
ENDF-6 formatted files.
2 Basic Objectives and Scope
The basic objectives of the EMPIRE code are:
• to provide the state-of-the-art modeling of nuclear reactions for basic science and
data evaluation;
• to ensure reasonably comprehensive coverage of incident particles, targets,
incident energies, and observables;
• To unify (1) reaction models, (2) model parameters, (3) nuclear structure data,
and (4) experimental results;
• to provide a full set of tools for evaluators to enable efficient production of high
quality nuclear data files;
• to be as general, flexible, and easy to use as possible.
The present scope of the code includes:
• A broad range of incident energies (up to 150 MeV) and projectiles (n, p, d, t,
3 He, 4 He, photons, and heavy ions);
• The low-energy range for neutron reactions covered by an interface to the Atlas
of Neutron Resonances [1];
• Default input parameters for targets of mass number A ≥ 20 [2];
• Direct, pre-equilibrium, and statistical model reaction mechanisms—with width
fluctuations and a full gamma cascade;
• Observables: cross sections, angular distributions, spectra (including prompt
fission neutron spectra), energy-angular distributions;
• Outgoing channels: multi-particle emission, γ -emission (including discrete
lines), discrete levels (including isomers), fission, several exclusive channels.
To a large extent, the present scope of the EMPIRE code permits it to fulfill its
objectives. However, it should also be clear that the objectives are an evolving target
that will never be completely met.