133,953 research outputs found

### Residue symbols and Jantzen-Seitz partitions

Jantzen-Seitz partitions are those $p$-regular partitions of~$n$ which label
$p$-modular irreducible representations of the symmetric group $S_n$ which
remain irreducible when restricted to $S_{n-1}$; they have recently also been
found to be important for certain exactly solvable models in statistical
mechanics. In this article we study their combinatorial properties via a
detailed analysis of their residue symbols; in particular the $p$-cores of
Jantzen-Seitz partitions are determined

### The hadron-quark transition with a lattice of nonlocal confining solitons

We use a lattice of nonlocal confining solitons to describe nuclear matter in
the Wigner-Seitz approximation. The average density is varied by changing the
size of the Wigner-Seitz cell. At sufficiently large density quark energy bands
develop. The intersection of the filled valence band with the next empty band
at a few times standard nuclear density signals a transition from a color
insulator to a color conductor and is identified with the critical density for
quark deconfinement.Comment: 12 pages Latex with one PS figur

### Equation of state in the inner crust of neutron stars: discusion of the unbound neutron states

In this paper, we calculate the stable Wigner-Seitz (W-S) cells in the inner
crust of neutron stars and we discuss the nuclear shell effects. A distinction
is done between the shell effects due to the bound states and those induced by
the unbound states, which are shown to be spurious. We then estimate the
effects of the spurious shells on the total energy and decompose it into a
smooth and a residual part. We propose a correction to the Hartree-Fock binding
energy in Wigner-Seitz cell (HF-WS).Comment: conference EXOCT07, Catania, 11-15 June, 200

### Exact energy of the spin-polarized two-dimensional electron gas at high density

We derive the exact expansion, to $O(r_s)$, of the energy of the high-density
spin-polarized two-dimensional uniform electron gas, where $r_s$ is the Seitz
radius.Comment: 7 pages, 1 figure and 1 table, submitted to Phys. Rev.

### The role of the boundary conditions in the Wigner-Seitz approximation applied to the neutron star inner crust

The influence of the boundary conditions used in the Wigner-Seitz
approximation applied to the neutron star inner crust is examined. The
generalized energy functional method which includes neutron and proton pairing
correlations is used. Predictions of two versions of the boundary conditions
are compared with each other. The uncertainties in the equilibrium
configuration (Z,R_c) of the crust, where Z is the proton charge and R_c the
radius of the Wigner-Seitz cell, correspond to variation of Z by 2 -- 6 units
and of R_c, by 1 -- 2 fm. The effect of the boundary conditions is enhanced at
increasing density. These uncertainties are smaller than the variation of Z and
R_c coming from the inclusion of pairing. The value of the pairing gap itself,
especially at high density, can depend on the boundary condition used.Comment: LaTeX, 11 pages, 3 figures, to be published in Phys. Lett.

### Collective excitations in the inner crust of neutron stars : supergiant resonances

We investigate the nuclear collective excitations of Wigner-Seitz cells
containing nuclear clusters immersed in a gas of neutrons. This baryonic
non-uniform system is specific to the structure of inner crust matter of
neutron stars. The collective excitations are studied in the framework of a
spherical Hartree-Fock-Bogoliubov + Quasiparticle Random Phase Approximation,
formulated in coordinate representation. The calculations are done for two
representative Wigner-Seitz cells with baryonic density equal to 0.02 fm$^{-3}$
and 0.08 fm$^{-3}$. It is shown that the excitations with low multipolarities
are concentrated almost entirely in one strongly collective mode which exhausts
a very large fraction of the energy-weighted sum rule. Since these collective
modes are located at very low energies compared to the giant resonances in
standard nuclei, they may affect significantly the specific heat of baryonic
inner crust matter of neutron stars.Comment: 6 pages, 4 figure

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