Equation of State of Superfluid Neutron Matter and the Calculation of the<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mmultiscripts><mml:mi>S</mml:mi><mml:mn>0</mml:mn><mml:none /><mml:mprescripts /><mml:none /><mml:mn>1</mml:mn></mml:mmultiscripts></mml:math>Pairing Gap

Gandolfi, Stefano; Illarionov, A. Yu.; Fantoni, S.; Pederiva, Francesco; Schmidt, Kevin

doi:10.1103/physrevlett.101.132501

Cited by 103 publications

(151 citation statements)

References 26 publications

Supporting

Mentioning

136

Contrasting

Order By: Relevance

“…A quantitative assessment of this effect requires all contributions to be treated consistently and represents the subject of a future work. Recently, ab initio quantum Monte Carlo calculations have been carried out for low-density infinite neutron matter (k F,n 0.5 fm −1 ) [48], with an effort to understand the differences with other Monte Carlo results [49][50][51]. A quenching of the mean-field pairing gap is predicted, resulting in a larger pairing gap than what previous calculations found [52][53][54][55][56].…”

Section: Discussionmentioning

confidence: 94%

Superfluid properties of the inner crust of neutron stars

2011

View full text Add to dashboard Cite

We investigated the superfluid properties of the inner crust of neutron stars, solving the Hartree-FockBogoliubov equations in spherical Wigner-Seitz cells. Using realistic two-body interactions in the pairing channel, we studied in detail the Cooper-pair and the pairing-field spatial properties, together with the effect of the proton clusters on the neutron pairing gap. Calculations with effective pairing interactions are also presented, showing significant discrepancies with the results obtained with realistic pairing forces. At variance with recent studies on finite nuclei, the neutron coherence length is found to depend on the strength of the pairing interaction, even inside the nucleus. We also show that the spherical Wigner-Seitz approximation breaks down in the innermost regions of the inner crust, already at baryonic densities ρ b 8 × 10 +13 g/cm 3 .

show abstract

Section: Discussionmentioning

confidence: 94%

Superfluid properties of the inner crust of neutron stars

2011

View full text Add to dashboard Cite

show abstract

“…For each value of L and for each zone of table 1 we have calculated the pinning force per unit length fL and the estimated error σ f L for two values of the polarization correction factor, β = 1 (i.e. the case of a bare interaction) and β = 3, which is close to the value obtained in realistic Montecarlo simulations of neutron matter (Gandolfi et al 2008). The results for the pinning force per unit length are also plotted in figure 10 for β = 1 and in figure 11 for β = 3.…”

Section: Results Of the Model: Bcc Latticementioning

confidence: 99%

“…When β = 1 the mean pairing gap has a maximum of about 3 MeV, which corresponds to the strong pairing scenario, while when β = 3 the mean pairing gap has a maximum of about 1 MeV, as usually assumed in the weak pairing scenario. Realistic Montecarlo simulations of neutron matter (Gandolfi et al 2008) indicate a reduction of the pairing gap consistent with the choice β = 3.…”

Section: Lattice Propertiesmentioning

confidence: 99%

Mesoscopic pinning forces in neutron star crusts

Seveso¹,

Pizzochero²,

Grill³

et al. 2015

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

The crust of a neutron star is thought to be comprised of a lattice of nuclei immersed in a sea of free electrons and neutrons. As the neutrons are superfluid their angular momentum is carried by an array of quantized vortices. These vortices can pin to the nuclear lattice and prevent the neutron superfluid from spinning down, allowing it to store angular momentum which can then be released catastrophically, giving rise to a pulsar glitch. A crucial ingredient for this model is the maximum pinning force that the lattice can exert on the vortices, as this allows us to estimate the angular momentum that can be exchanged during a glitch. In this paper we perform, for the first time, a detailed and quantitative calculation of the pinning force per unit length acting on a vortex immersed in the crust and resulting from the mesoscopic vortexlattice interaction. We consider realistic vortex tensions, allow for displacement of the nuclei and average over all possible orientation of the crystal with respect to the vortex. We find that, as expected, the mesoscopic pinning force becomes weaker for longer vortices and is generally much smaller than previous estimates, based on vortices aligned with the crystal. Nevertheless the forces we obtain still have maximum values of order f pin ≈ 10 15 dyn/cm, which would still allow for enough angular momentum to be stored in the crust to explain large Vela glitches, if part of the star is decoupled during the event.

show abstract

“…However, it seems very difficult at present in spite of recent progress toward this direction [12,27,28,29,30,31,32,33,34,35].…”

Section: Introductionmentioning

confidence: 99%

Optimal pair density functional for the description of nuclei with large neutron excess

2009

View full text Add to dashboard Cite

Toward a universal description of pairing properties in nuclei far from stability, we extend the energy density functional by enriching the isovector density dependence in the particle-particle channel (pair density functional, pair-DF). We emphasize the necessity of both the linear and quadratic isovector density terms. The parameters are optimized by the Hartree-Fock-Bogoliubov calculation for 156 nuclei of the mass number A = 118 − 196 and the asymmetry parameter (N − Z)/A < 0.25. We clarify that the pair-DF should include the isovector density dependence in order to take into account the effect of the isoscalar and isovector effective masses in the particle-hole channel consistently. The different Skyrme forces can give the small difference in the pairing gaps toward the neutron drip line, if the optimal pair-DF consistent with the particle-hole channel is employed.

show abstract

Equation of State of Superfluid Neutron Matter and the Calculation of theS01Pairing Gap

Cited by 103 publications

References 26 publications

Superfluid properties of the inner crust of neutron stars

Superfluid properties of the inner crust of neutron stars

Mesoscopic pinning forces in neutron star crusts

Optimal pair density functional for the description of nuclei with large neutron excess

Contact Info

Product

Resources

About