Renormalization group approach to neutron matter: quasiparticle interactions, superfluid gaps and the equation of state

By A. Schwenk, B. Friman, G. Brook, Gsi. 2002

135 citations recorded by the source corpus.

Renormalization group methods can be applied to the nuclear many-body problem using the approach proposed by Shankar. We start with the two-body low momentum interaction Vlowk and use the RG flow from the particle–hole channels to calculate the full scattering amplitude in the vicinity of the Fermi surface. This is a new straightforward approach to the many-body problem which is applicable also to condensed matter systems without long-range interactions, such as liquid 3He. We derive the one-loop renormalization group equations for the quasiparticle interaction and the scattering amplitude at zero temperature. The RG presents an elegant method to maintain all momentum scales and preserve the antisymmetry of the scattering amplitude. As a first application we solve the RG equations for neutron matter. The resulting quasiparticle interaction includes effects due to the polarization of the medium, the so-called induced interaction of Babu and Brown. We present results for the Fermi liquid parameters, the equation of state of neutron matter and the 1S0 superfluid pairing gap.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/8e5cc1398a12f6432cd9f4521d42912013b30558

How researchers see this paper

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In Astronomy and Astrophysics

1. J. Macbeth
2. D. Page
3. Armen Sedrakian
4. John W. Clark Jr.
5. A. Cumming
6. J. I. Zand
7. M. Zechmeister
8. M. Kürster

In Atomic and Molecular Physics, and Optics

1. Armen Sedrakian
2. John W. Clark Jr.

In Nuclear and High Energy Physics

1. D. Page
2. Armen Sedrakian
3. John W. Clark Jr.

Citations in the corpus

• Superfluidity in nuclear systems and neutron stars (2018, methodology): “We turn now to studies that employ more refined approximations for the induced part of the interaction [145– 147, 162].”
• Long Type I X-Ray Bursts and Neutron Star Interior Physics (2005, methodology): “[C5]), and we take the neutron 1S0 critical temperature Tc as a function of density as given by the calculation of Schwenk et al. (2003).”