Quasiparticle interactions in neutron matter for applications in neutron stars

doi:10.1016/0375-9474(93)90317-Q

Nuclear Physics A

Volume 555, Issue 1, 5 April 1993, Pages 128-150

https://doi.org/10.1016/0375-9474(93)90317-Q Get rights and content

Abstract

A microscopic model for the quasiparticle interaction in neutron matter is presented. Both particle-particle (pp) and particle-hole (ph) correlations are included. The pp correlations are treated in a semi-empirical way, while ph correlations are incorporated by solving coupled two-body equations for the particle-hole interaction and the scattering amplitude on the Fermi sphere. The resulting integral equations self-consistently sum the ph reducible diagrams. Antisymmetry is kept at all stages and hence the forward-scattering sum rules for the scattering amplitude are obeyed. Results for Landau parameters and transport coefficients in a density regime representing the crust of a neutron star are presented. We also estimate the ¹S₀ gap parameter for neutron superfluidity and comment briefly on neutron-star implications.

References (37)

D.B. Kaplan et al.
Phys. Lett.
(1986)
T.L. Ainsworth et al.
Phys. Lett.
(1989)
D. Pines et al.
Nucl. Phys.
(1988)
O. Sjöberg
Ann. of Phys.
(1973)
S. Babu et al.
Ann. of Phys.
(1973)
S.-O. Bäckman et al.
Phys. Reports
(1985)
B. Friedman et al.
Nucl. Phys.
(1981)
A.D. Jackson et al.
Nucl. Phys.
(1982)
J.A. Niskanen and J.A. Sauls, preprint...
J. Bardeen et al.
Phys. Rev.
(1957)

J.M.C. Chen et al.

Nucl. Phys.

(1986)

D. PinesJ.W. Clark et al.

Phys. Lett.

(1976)

J.W. Clark, R.D. Davé and J.M.C. Chen, to be...

A.B. Migdal

Rev. Mod. Phys.

(1978)

A.B. Migdal

Sov. Phys. JETP

(1960)

D. Pines et al.

Nature

(1985)

M.A. Alpar et al.

Astrophys. J.

(1985)

O.V. Maxwell

Astrophys. J.

(1979)

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^☆: This paper is dedicated to the memory of A.B. Migdal.

¹: Present address: Institut für Kernphysik, Forschungszentrum Jülich, D-5170 Jülich, Germany.

²: Present address: Department of Physics, Texas A&M University, College Station, TX 77843, USA.

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Quasiparticle interactions in neutron matter for applications in neutron stars☆

Abstract

Phys. Lett.

Phys. Lett.

Nucl. Phys.

Ann. of Phys.

Ann. of Phys.

Phys. Reports

Nucl. Phys.

Nucl. Phys.

Phys. Rev.

Nucl. Phys.

Phys. Lett.

Rev. Mod. Phys.

Sov. Phys. JETP

Nature

Astrophys. J.

Astrophys. J.