|
Next revision
|
Previous revision
|
aswns [2022/08/16 07:11]
theoastro created |
aswns [2022/08/16 20:55] (current)
theoastro [Further documentation:] |
| ====== ASWNS ====== | ====== ASWNS ====== |
| |
| ASWNS stands for "Arcetri-Stockholm-Warsaw Neutron Stars". The code was mainly developed by G. Camelio, is an extension of the [[XNS-v2 code|https://arxiv.org/abs/1401.4308]] , and computes rotating neutron star configurations using the extended Conformal Flatness approximation and is written in FORTRAN 90. | ==== Summary ==== |
| | |
| | ASWNS stands for "Arcetri-Stockholm-Warsaw Neutron Stars". The code was mainly developed by G. Camelio, is an extension of the [[https://arxiv.org/abs/1401.4308|XNS-v2 code]] , and computes rotating neutron star configurations using the extended Conformal Flatness approximation and is written in FORTRAN 90. |
| The main assumptions used in the code are stationarity, axisymmetry, and circularity (the matter motion is purely toroidal) of the solution. However, the rotation profile can be generic, i.e., both rigid and differential rotation are supported, and it is possible to use a cold, hot, barotropic, or baroclinic equation of state. | The main assumptions used in the code are stationarity, axisymmetry, and circularity (the matter motion is purely toroidal) of the solution. However, the rotation profile can be generic, i.e., both rigid and differential rotation are supported, and it is possible to use a cold, hot, barotropic, or baroclinic equation of state. |
| |
| ASWNS has been used for a variety of tasks, namely: | ASWNS has been used for a variety of tasks, namely: |
| * [[for computing the ejecta mass after the collapse of a cold, rigid-rotating neutron star|https://arxiv.org/abs/1806.07775]] | * [[https://arxiv.org/abs/1806.07775|for computing the ejecta mass after the collapse of a cold, rigid-rotating neutron star]] |
| * [[to study baroclinic neutron star configurations|https://arxiv.org/abs/1908.11258]] | * [[https://arxiv.org/abs/1908.11258|to study baroclinic neutron star configurations]] |
| * [[to model hot, nonbarotropic, differentially rotating neutron star merger remnants|https://arxiv.org/abs/2011.10557]] | * [[https://arxiv.org/abs/2011.10557|to model hot, nonbarotropic, differentially rotating neutron star merger remnants]] |
| | |
| | ==== Further documentation: ==== |
| | * [[Installation_ASWNS|Installation]] |
| | * [[Examples_ASWNS|Examples (non-barotropic stars and configurations at the Kepler limit)]] |
| | * [[general_aswns|General settings]] |
