Finite size effects in neutron star and nuclear matter simulations
In this work we study molecular dynamics simulations of symmetric nuclear and neutron star matter using a semi-classical nucleon interaction model. Our aim is to gain insight on the nature of the so-called "finite size effects", unavoidable in this kind of simulations, and to understand wh...
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| Acceso en línea: | https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_03759474_v933_n_p306_GimenezMolinelli http://hdl.handle.net/20.500.12110/paper_03759474_v933_n_p306_GimenezMolinelli |
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paper:paper_03759474_v933_n_p306_GimenezMolinelli2023-06-08T15:38:22Z Finite size effects in neutron star and nuclear matter simulations Dorso, Claudio Oscar Finite size effects Molecular dynamics simulations Nuclear astrophysics Nuclear matter phase transition In this work we study molecular dynamics simulations of symmetric nuclear and neutron star matter using a semi-classical nucleon interaction model. Our aim is to gain insight on the nature of the so-called "finite size effects", unavoidable in this kind of simulations, and to understand what they actually affect. To do so, we explore different geometries for the periodic boundary conditions imposed on the simulation cell: cube, hexagonal prism and truncated octahedron. For nuclear matter simulations we show that, at sub-saturation densities and low temperatures, the solutions are non-homogeneous structures reminiscent of the "nuclear pasta" phases expected in neutron star matter simulations, but only one structure per cell and shaped by specific artificial aspects of the simulations-for the same physical conditions (i.e. number density and temperature) different cells yield different solutions. The particular shape of the solution at low enough temperature and a given density can be predicted analytically by surface minimization. We also show that even if this behavior is due to the imposition of periodic boundary conditions on finite systems, this does not mean that it vanishes for very large systems, and it is actually independent of the system size. We conclude that, for nuclear matter simulations, the cells' size sets the only characteristic length scale for the inhomogeneities, and the geometry of the periodic cell determines the shape of those inhomogeneities.To model neutron star matter we add a screened Coulomb interaction between protons, and perform simulations in the three cell geometries. Our simulations indeed produce the well known nuclear pasta, with (in most cases) several structures per cell. However, we find that for systems not too large results are affected by finite size in different ways depending on the geometry of the cell. In particular, at the same certain physical conditions and system size, the hexagonal prism yields a single structure per cell while the cubic and truncated octahedron show consistent results, with more than one structure per cell. For systems of the size studied in this work these effects are still noticeable, but we find evidence to support that the dependence of the results on the cell geometry becomes smaller as the system size is increased. When the Coulomb interaction is present, the competition between opposing interactions of different range results in a proper, physically meaningful length scale that is independent of the system size and periodic cell of choice. Only under these conditions "finite size effects" will vanish for large enough systems (i.e. cells much larger than this characteristic length). Larger simulations are in order, but our computational capabilities forbid it for the time being. © 2014 Elsevier B.V.. Fil:Dorso, C.O. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. 2015 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_03759474_v933_n_p306_GimenezMolinelli http://hdl.handle.net/20.500.12110/paper_03759474_v933_n_p306_GimenezMolinelli |
| institution |
Universidad de Buenos Aires |
| institution_str |
I-28 |
| repository_str |
R-134 |
| collection |
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) |
| topic |
Finite size effects Molecular dynamics simulations Nuclear astrophysics Nuclear matter phase transition |
| spellingShingle |
Finite size effects Molecular dynamics simulations Nuclear astrophysics Nuclear matter phase transition Dorso, Claudio Oscar Finite size effects in neutron star and nuclear matter simulations |
| topic_facet |
Finite size effects Molecular dynamics simulations Nuclear astrophysics Nuclear matter phase transition |
| description |
In this work we study molecular dynamics simulations of symmetric nuclear and neutron star matter using a semi-classical nucleon interaction model. Our aim is to gain insight on the nature of the so-called "finite size effects", unavoidable in this kind of simulations, and to understand what they actually affect. To do so, we explore different geometries for the periodic boundary conditions imposed on the simulation cell: cube, hexagonal prism and truncated octahedron. For nuclear matter simulations we show that, at sub-saturation densities and low temperatures, the solutions are non-homogeneous structures reminiscent of the "nuclear pasta" phases expected in neutron star matter simulations, but only one structure per cell and shaped by specific artificial aspects of the simulations-for the same physical conditions (i.e. number density and temperature) different cells yield different solutions. The particular shape of the solution at low enough temperature and a given density can be predicted analytically by surface minimization. We also show that even if this behavior is due to the imposition of periodic boundary conditions on finite systems, this does not mean that it vanishes for very large systems, and it is actually independent of the system size. We conclude that, for nuclear matter simulations, the cells' size sets the only characteristic length scale for the inhomogeneities, and the geometry of the periodic cell determines the shape of those inhomogeneities.To model neutron star matter we add a screened Coulomb interaction between protons, and perform simulations in the three cell geometries. Our simulations indeed produce the well known nuclear pasta, with (in most cases) several structures per cell. However, we find that for systems not too large results are affected by finite size in different ways depending on the geometry of the cell. In particular, at the same certain physical conditions and system size, the hexagonal prism yields a single structure per cell while the cubic and truncated octahedron show consistent results, with more than one structure per cell. For systems of the size studied in this work these effects are still noticeable, but we find evidence to support that the dependence of the results on the cell geometry becomes smaller as the system size is increased. When the Coulomb interaction is present, the competition between opposing interactions of different range results in a proper, physically meaningful length scale that is independent of the system size and periodic cell of choice. Only under these conditions "finite size effects" will vanish for large enough systems (i.e. cells much larger than this characteristic length). Larger simulations are in order, but our computational capabilities forbid it for the time being. © 2014 Elsevier B.V.. |
| author |
Dorso, Claudio Oscar |
| author_facet |
Dorso, Claudio Oscar |
| author_sort |
Dorso, Claudio Oscar |
| title |
Finite size effects in neutron star and nuclear matter simulations |
| title_short |
Finite size effects in neutron star and nuclear matter simulations |
| title_full |
Finite size effects in neutron star and nuclear matter simulations |
| title_fullStr |
Finite size effects in neutron star and nuclear matter simulations |
| title_full_unstemmed |
Finite size effects in neutron star and nuclear matter simulations |
| title_sort |
finite size effects in neutron star and nuclear matter simulations |
| publishDate |
2015 |
| url |
https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_03759474_v933_n_p306_GimenezMolinelli http://hdl.handle.net/20.500.12110/paper_03759474_v933_n_p306_GimenezMolinelli |
| work_keys_str_mv |
AT dorsoclaudiooscar finitesizeeffectsinneutronstarandnuclearmattersimulations |
| _version_ |
1768545787520745472 |