Abstract:In this Review we study the nuclear pastas as they are expected to be formed in neutron star cores. We start with a study of the pastas formed in nuclear matter (composed of protons and neutrons), we follow with the role of the electron gas on the formation of pastas, and we then investigate the pastas in neutron star matter (nuclear matter embedded in an electron gas).
Nuclear matter (NM) at intermediate temperatures (1 MeVT 15 MeV), at saturation and sub-saturation densities, and with proton content ranging … Show more
“…versus density that we can see from figure 4 is in accordance with what has been obtained in numerical simulations of nuclear pasta (see [12]). In fact, the above is one of the main goals of the present work: relevant features of the nuclear pasta state, that until now has only been possible to study numerically, can be characterized from analytical solutions of the SU(N )-Skyrme model.…”
Section: Jhep12(2021)150supporting
confidence: 91%
“…Thus, the first family is suitable to describe nuclear spaghetti while the second family to describe nuclear lasagna. Indeed, on the nuclear spaghetti side, the similarity of the contour plots in [40] with the spaghetti-like configurations found (numerically) in the nuclear pasta phase (see the plots in [1][2][3][4][5] and [12]) is quite remarkable. On the nuclear lasagna side, the contour plots of the energy density and Baryon density, which can be found using the results in [39], are JHEP12(2021)150 very close to the numerical plots in [1][2][3][4][5], for the lasagna case.…”
Section: Introductionmentioning
confidence: 62%
“…We show all the allowed configurations with B = 20 and p = 1. One can see that the behavior of the curves has the characteristic "u-shape" of nuclear pasta shown in [12].…”
Section: Jhep12(2021)150mentioning
confidence: 87%
“…One of the most fascinating phenomena appearing when a large amount of Baryon charge is present within a finite volume (which has been confirmed both phenomenologically and with numerical simulations) is the appearance of ordered structures called nuclear pasta phase (see [1][2][3][4][5][6][7][8][9][10][11] and the nice up to date review [12]). Two of the most studied shapes are nuclear spaghetti (in which most of the Baryonic charge lies within tube-shaped region) and nuclear lasagna (in which most of the Baryonic charge lies within layers of finite width).…”
Section: Introductionmentioning
confidence: 86%
“…In fact, the comparison between the magnetic field decay of neutron stars and their corresponding spin evolution obtained by numerical methods in references [54] and [55], suggests that such structures exist. In the light of the fact that lasagna and spaghetti phases are expected to have quite different physical properties (see [12] and references therein).…”
We construct explicit analytic solutions of the SU(N)-Skyrme model (for generic N) suitable to describe different phases of nuclear pasta at finite volume in (3 + 1) dimensions. The first type are crystals of Baryonic tubes (nuclear spaghetti) while the second type are smooth Baryonic layers (nuclear lasagna). Both, the ansatz for the spaghetti and the ansatz for the lasagna phases, reduce the complete set of Skyrme field equations to just one integrable equation for the profile within sectors of arbitrary high topological charge. We compute explicitly the total energy of both configurations in terms of the flavor number, the density and the Baryonic charge. Remarkably, our analytic results allow to compare explicitly the physical properties of nuclear spaghetti and lasagna phases. Our construction shows explicitly that, at lower densities, configurations with N = 2 light flavors are favored while, at higher densities, configurations with N = 3 are favored. Our construction also proves that in the high density regime (but still well within the range of validity of the Skyrme model) the lasagna configurations are favored while at low density the spaghetti configurations are favored. Moreover, the integrability property of the present configurations is not spoiled by the inclusion of the subleading corrections to the Skyrme model arising in the ’t Hooft expansion. Finally, we briefly discuss the large N limit of our configurations.
“…versus density that we can see from figure 4 is in accordance with what has been obtained in numerical simulations of nuclear pasta (see [12]). In fact, the above is one of the main goals of the present work: relevant features of the nuclear pasta state, that until now has only been possible to study numerically, can be characterized from analytical solutions of the SU(N )-Skyrme model.…”
Section: Jhep12(2021)150supporting
confidence: 91%
“…Thus, the first family is suitable to describe nuclear spaghetti while the second family to describe nuclear lasagna. Indeed, on the nuclear spaghetti side, the similarity of the contour plots in [40] with the spaghetti-like configurations found (numerically) in the nuclear pasta phase (see the plots in [1][2][3][4][5] and [12]) is quite remarkable. On the nuclear lasagna side, the contour plots of the energy density and Baryon density, which can be found using the results in [39], are JHEP12(2021)150 very close to the numerical plots in [1][2][3][4][5], for the lasagna case.…”
Section: Introductionmentioning
confidence: 62%
“…We show all the allowed configurations with B = 20 and p = 1. One can see that the behavior of the curves has the characteristic "u-shape" of nuclear pasta shown in [12].…”
Section: Jhep12(2021)150mentioning
confidence: 87%
“…One of the most fascinating phenomena appearing when a large amount of Baryon charge is present within a finite volume (which has been confirmed both phenomenologically and with numerical simulations) is the appearance of ordered structures called nuclear pasta phase (see [1][2][3][4][5][6][7][8][9][10][11] and the nice up to date review [12]). Two of the most studied shapes are nuclear spaghetti (in which most of the Baryonic charge lies within tube-shaped region) and nuclear lasagna (in which most of the Baryonic charge lies within layers of finite width).…”
Section: Introductionmentioning
confidence: 86%
“…In fact, the comparison between the magnetic field decay of neutron stars and their corresponding spin evolution obtained by numerical methods in references [54] and [55], suggests that such structures exist. In the light of the fact that lasagna and spaghetti phases are expected to have quite different physical properties (see [12] and references therein).…”
We construct explicit analytic solutions of the SU(N)-Skyrme model (for generic N) suitable to describe different phases of nuclear pasta at finite volume in (3 + 1) dimensions. The first type are crystals of Baryonic tubes (nuclear spaghetti) while the second type are smooth Baryonic layers (nuclear lasagna). Both, the ansatz for the spaghetti and the ansatz for the lasagna phases, reduce the complete set of Skyrme field equations to just one integrable equation for the profile within sectors of arbitrary high topological charge. We compute explicitly the total energy of both configurations in terms of the flavor number, the density and the Baryonic charge. Remarkably, our analytic results allow to compare explicitly the physical properties of nuclear spaghetti and lasagna phases. Our construction shows explicitly that, at lower densities, configurations with N = 2 light flavors are favored while, at higher densities, configurations with N = 3 are favored. Our construction also proves that in the high density regime (but still well within the range of validity of the Skyrme model) the lasagna configurations are favored while at low density the spaghetti configurations are favored. Moreover, the integrability property of the present configurations is not spoiled by the inclusion of the subleading corrections to the Skyrme model arising in the ’t Hooft expansion. Finally, we briefly discuss the large N limit of our configurations.
It is show that one can derive a novel BPS bound for the gauged Non-Linear-Sigma-Model (NLSM) Maxwell theory in (3+1) dimensions which can actually be saturated. Such novel bound is constructed using Hamilton-Jacobi equation from classical mechanics. The configurations saturating the bound represent Hadronic layers possessing both Baryonic charge and magnetic flux. However, unlike what happens in the more common situations, the topological charge which appears naturally in the BPS bound is a non-linear function of the Baryonic charge. This BPS bound can be saturated when the surface area of the layer is quantized. The far-reaching implications of these results are discussed. In particular, we determine the exact relation between the magnetic flux and the Baryonic charge as well as the critical value of the Baryonic chemical potential beyond which these configurations become thermodynamically unstable.
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