Transport Properties of the Nuclear Pasta Phase with Quantum Molecular Dynamics

Nandi, Rana; Schramm, Stefan

doi:10.3847/1538-4357/aa9f12

Cited by 36 publications

(46 citation statements)

References 46 publications

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“…As such, the static response functions of neutrino and electron scattering with pasta have been previously calculated in several simulations [76][77][78][79][80][81][82][83]. We apply the Quantum Molecular Dynamics simulation results [84], as these are relevant for our stellar temperatures and dark matter momentum transfers. These simulations capture the coherence effects of interacting with the whole pasta structure.…”

Section: Scattering With Nuclear Pastamentioning

confidence: 99%

Warming nuclear pasta with dark matter: kinetic and annihilation heating of neutron star crusts

Acevedo

Bramante

Leane

et al. 2020

J. Cosmol. Astropart. Phys.

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Neutron stars serve as excellent next-generation thermal detectors of dark matter, heated by the scattering and annihilation of dark matter accelerated to relativistic speeds in their deep gravitational wells. However, the dynamics of neutron star cores are uncertain, making it difficult at present to unequivocally compute dark matter scattering in this region. On the other hand, the physics of an outer layer of the neutron star, the crust, is more robustly understood. We show that dark matter scattering solely with the low-density crust still kinetically heats neutron stars to infrared temperatures detectable by forthcoming telescopes. We find that for both spin-independent and spin-dependent scattering on nucleons, the crust-only cross section sensitivity is 10 −43 − 10 −41 cm 2 for dark matter masses of 100 MeV − 1 PeV, with the best sensitivity arising from dark matter scattering with a crust constituent called nuclear pasta (including gnocchi, spaghetti, and lasagna phases). For dark matter masses from 10 eV to 1 MeV, the sensitivity is 10 −39 − 10 −34 cm 2 , arising from exciting collective phonon modes in a neutron superfluid in the inner crust. Furthermore, for any s-wave or p-wave annihilating dark matter, we show that dark matter will efficiently annihilate by thermalizing just with the neutron star crust, regardless of whether the dark matter ever scatters with the neutron star core. This implies efficient annihilation in neutron stars for any electroweakly interacting dark matter with inelastic mass splittings of up to 200 MeV, including Higgsinos. We conclude that neutron star crusts play a key role in dark matter scattering and annihilation in neutron stars. *

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Section: Scattering With Nuclear Pastamentioning

confidence: 99%

Warming nuclear pasta with dark matter: kinetic and annihilation heating of neutron star crusts

Acevedo

Bramante

Leane

et al. 2020

J. Cosmol. Astropart. Phys.

View full text Add to dashboard Cite

show abstract

“…Nuclear pasta has been the topic of research for some decades [1,2] and has been much studied with classical [3,4] and quantum methods [5][6][7][8][9][10][11][12][13][14][15][16][17]. The impact of pasta matter on astrophysical objects are manifold: the viscosity of pasta matter can dampen the oscillations of neutron stars, its thermal conductivity is important for the neutron star cooling [18], it can explain the limitation of spin periods of pulsars [19] and its neutrino opacity has an impact on the early stage of cooling of the neutron star and the explodability of supernovae [20][21][22][23][24][25]. In this paper, we focus on neutrino scattering and the impact of pasta structures on neutrino opacities.…”

Section: Introductionmentioning

confidence: 99%

“…These can have a significant impact on the opacities and thus on the astrophysical scenarios. For explicit nuclear pasta configurations the neutrino opacity has only been studied using the molecular dynamics (MD) framework [20][21][22]25]. MD has the advantage that it includes real particle-particle correlations between nucleons.…”

Section: Introductionmentioning

confidence: 99%

Survey of nuclear pasta in the intermediate-density regime: Shapes and energies

Schuetrumpf¹,

Martı́nez-Pinedo²,

Afibuzzaman³

et al. 2019

Phys. Rev. C

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Background: Nuclear pasta matter, emerging due to the competition between the long-range Coulomb force and the short-range strong force, is believed to be present in astrophysical scenarios, such as neutron stars and corecollapse supernovae. Its structure can have a high impact e.g. on neutrino transport or the tidal deformability of neutron stars.Purpose: We investigate the impact of nuclear pasta on neutrino interactions and compare the results to uniform matter.Method: We calculate the elastic and inelastic static structure factors for nuclear pasta matter using density functional theory (DFT), which contain the main nuclear input for neutrino scattering.Results: Each pasta structure leaves a unique imprint in the elastic structure factor and it is largely enhanced. The inelastic structure factors are very similar for all configurations.Conclusion: Nuclear pasta has a noticeable impact on neutrino neutral-current scattering opacities. While for inelastic reactions the cross section is reduced, the elastic coherent scattering increases dramatically. The effect can be of importance for the cooling of neutron stars as well as for core-collapse supernova models.

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“…Complex structures (e.g., rod, slab, bubble, etc. -collectively known as nuclear pasta) are expected to occur in the inner crust as the matter gradually changes from crystalline to homogeneous phase, with increasing density [26][27][28][29] . Beneath the inner crust, the outer core starts, with uniform nuclear matter.…”

Section: Introductionmentioning

confidence: 99%

Role of crustal physics in the tidal deformation of a neutron star

et al. 2019

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In the late inspiral phase, gravitational waves from binary neutron star mergers carry the imprint of the equation of state due to the tidally deformed structure of the components. If the stars contain solid crusts, then their shear modulus can affect the deformability of the star and, thereby, modify the emitted signal. Here, we investigate the effect of realistic equations of state (EOSs) of the crustal matter, with a realistic model for the shear modulus of the stellar crust in a fully general relativistic framework. This allows us to systematically study the deviations that are expected from fluid models. In particular, we use unified EOSs, both relativistic and non-relativistic, in our calculations. We find that realistic EOSs of crusts cause a small correction, of ∼ 1%, in the second Love number. This correction will likely be subdominant to the statistical error expected in LIGO-Virgo observations at their respective advanced design sensitivities, but rival that error in third generation detectors. For completeness, we also study the effect of crustal shear on the magnetic-type Love number and find it to be much smaller.

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Transport Properties of the Nuclear Pasta Phase with Quantum Molecular Dynamics

Cited by 36 publications

References 46 publications

Warming nuclear pasta with dark matter: kinetic and annihilation heating of neutron star crusts

Warming nuclear pasta with dark matter: kinetic and annihilation heating of neutron star crusts

Survey of nuclear pasta in the intermediate-density regime: Shapes and energies

Role of crustal physics in the tidal deformation of a neutron star

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