Calculation of the transport coefficients of the nuclear pasta phase

Nandi, Rana; Schramm, Stefan

doi:10.1007/s12036-018-9533-6

Cited by 18 publications

(18 citation statements)

References 24 publications

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“…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: 87%

“…On the other hand the energy-momentum tensor of the theory including the subleading corrections is T µν = T Sk µν + T (6) µν + T (8) µν , (…”

Section: Jhep12(2021)150mentioning

confidence: 99%

“…The properties of nuclear pasta attracted a lot of attention recently (see [6][7][8][13][14][15]] and references therein), but, due to both the very large Baryon number typical of this phase as well as to the strong interactions between them, only numerical results are available. Moreover, to obtain meaningful numerical results is extremely challenging in these complex JHEP12(2021)150 systems and a very high computing power is required (as it can be deduced from the references mentioned above).…”

Section: Introductionmentioning

confidence: 99%

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Analytic multi-Baryonic solutions in the SU(N)-Skyrme model at finite density

Cacciatori

Canfora

Lagos

et al. 2021

J. High Energ. Phys.

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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.

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Section: Introductionmentioning

confidence: 87%

“…On the other hand the energy-momentum tensor of the theory including the subleading corrections is T µν = T Sk µν + T (6) µν + T (8) µν , (…”

Section: Jhep12(2021)150mentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Analytic multi-Baryonic solutions in the SU(N)-Skyrme model at finite density

Cacciatori

Canfora

Lagos

et al. 2021

J. High Energ. Phys.

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“…At a high temperature of a proto-neutron star, thermal fluctuations should cause deviations from the regular structure and accordingly suppression of conductivities not only for the pasta phases but also for the spherical nuclei. Indeed, MD simulations by Nandi & Schramm (2018) suggest that the structure factors and hence conductivities in the pasta phase do not substantially differ from those in the ordinary phase of quasi-spherical nuclei at the same temperature.…”

Section: The Effect Of Crust Impurities On Conductivitiesmentioning

confidence: 99%

Crust structure and thermal evolution of neutron stars in soft X-ray transients

Potekhin

Chabrier

2021

A&A

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Context. Thermal evolution of neutron stars in soft X-ray transients (SXTs) is sensitive to the equation of state, nucleon superfluidity, composition and structure of the crust. Comparison of observations of their crust cooling with simulations is a powerful tool of verification of theoretical models of the dense matter. Aims. We study the effect of physics input on thermal evolution of neutron stars in SXTs. In particular, we consider different modern models of the sources of deep crustal heating during accretion episodes and the effects brought about by impurities embedded in the crust during its formation. Methods. We simulate thermal structure and evolution of episodically accreting neutron stars under different assumptions on the crust composition and on the distribution of heat sources and impurities. For the nonaccreted crust, we consider the nuclear charge fluctuations that arise at crust formation. For the accreted crust, we compare different theoretical models of composition and internal heating. We also compare results of numerical simulations with observations of the crust cooling in SXT MXB 1659−29. Results. The nonaccreted part of the inner crust of a neutron star can have a layered structure, with almost pure crystalline layers interchanging with layers composed of mixtures of different nuclei. The latter layers have relatively low thermal conductivities, which affects thermal evolution of the transients. The impurity distribution in the crust strongly depends on the models of the dense matter and the crust formation scenario. The shallow heating that is needed to reach agreement between the theory and observations depends on characteristics of the crust and envelope.

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“…During literature survey, we get a long list of references [40,41,42,43,44,45,46,47,48,49,50,51,52,53,54,55,56,57,58,59], concentrated on microscopic calculation of transport coefficients for NS system. In terms of specific contribution, sketching the thermodynamical phase space of transport coefficients with respect to density may be considered as an alternative portrait, relevant for qualitative understanding hadron-quark transition in astrophysical environment.…”

Section: Introductionmentioning

confidence: 99%

Estimation of transport coefficients of dense hadronic and quark matter

Sen,

Alam,

Ghosh

2021

Preprint

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We have attempted to visualize transport coefficients like shear viscosity and electrical conductivity with respect to density of neutron star environment, whose core may expect a hadron-quark phase transition due to acquiring much higher density than nuclear saturation density. By making sandwich between MIT bag model for quark phase and two different effective hadronic models for hadronic phase, we have estimated the transport coefficients of two phases. During sketching of the transport coefficients, we have discussed their detailed density profile of phase-space part and relaxation time part. By calculating shear viscosity to density ratio, we have also explored the nearly perfect fluid domain along the density axis of hadron-quark phase diagram.

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Calculation of the transport coefficients of the nuclear pasta phase

Cited by 18 publications

References 24 publications

Analytic multi-Baryonic solutions in the SU(N)-Skyrme model at finite density

Analytic multi-Baryonic solutions in the SU(N)-Skyrme model at finite density

Crust structure and thermal evolution of neutron stars in soft X-ray transients

Estimation of transport coefficients of dense hadronic and quark matter

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