Chiral three-nucleon forces and neutron matter

By K. Hebeler, A. Schwenk. 2009

238 citations recorded by the source corpus.

We calculate the properties of neutron matter and highlight the physics of chiral three-nucleon forces. For neutrons, only the long-range 2pi-exchange interactions of the leading chiral three-nucleon forces contribute, and we derive density-dependent two-body interactions by summing the third particle over occupied states in the Fermi sea. Our results for the energy suggest that neutron matter is perturbative at nuclear densities. We study in detail the theoretical uncertainties of the neutron matter energy, provide constraints for the symmetry energy and its density dependence, and explore the impact of chiral three-nucleon forces on the S-wave superfluid pairing gap.

View Paper: https://www.semanticscholar.org/paper/314159f5f78c2c34bf33ef46ee89ed98a7bed92a

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

Citations in the corpus

Symmetry energy impact in simulations of core-collapse supernovae (2013, methodology): “s supernova simulations via the nuclear matter EOS. In this article we review most of the currently used EOS for supernova matter. Moreover, recent constraints from Chiral Eective Field theory (EFT) [14,15,16,17,18,19,20] allow us to favor several of these supernova EOSs above others. Unfortunately,”
Symmetry Parameter Constraints from a Lower Bound on Neutron-matter Energy (2016, methodology): “…Quantum Monte Carlo (QMC) calculations (Gezerlis & Carlson 2010; Gandolfi et al. 2012; Lynn et al. 2016), many-body perturbation theory (MBPT) calculations (Hebeler & Schwenk 2010; Tews et al. 2013), and variational methods (Friedman & Pandharipande 1981; Akmal et al. 1998; Togashi & Takano 2013).”
Constraining the Speed of Sound inside Neutron Stars with Chiral Effective Field Theory Interactions and Observations (2018, methodology): “…interaction is unphysical and should be discarded for the following reasons: (i) the full N2LO 3N contributions in momentum-space calculations by Hebeler & Schwenk (2010), Tews et al. (2013), Hagen et al. (2014), Sammarruca et al. (2015), Wlazowski et al. (2014), and Drischler et al. (2016)…”
Equation of state sensitivities when inferring neutron star and dense matter properties (2018, methodology): “…speed of sound we employ a logistic function, which at low densities is matched to the theoretical calculations of neutron star matter performed in Hebeler & Schwenk (2010) and Hebeler et al. (2013) using nuclear interactions based on chiral effective field theory (cEFT) (Epelbaum, Hammer &…”
A NICER View of PSR J0030+0451: Implications for the Dense Matter Equation of State (2019, methodology): “These parameterizations were matched at 1.1ρs to either the upper limit or the lower limit of a calculated EoS range based on chiral effective field theory (cEFT) interactions including theoretical uncertainties (for details, see Hebeler & Schwenk 2010; Hebeler et al. 2013).”
Constraining the Dense Matter Equation of State with Joint Analysis of NICER and LIGO/Virgo Measurements (2019, methodology): “Both models are matched to an additional polytrope below 1.1n0 (with saturation density n0 = 0.16 fm −3) with varying normalization that captures the range of allowed EOS calculated from chiral effective field theory (chiral EFT) interactions (Hebeler & Schwenk 2010; Hebeler et al. 2013).”
Unified equation of state for neutron stars on a microscopic basis (2015, background): “…(Weinberg 1968, 1990, 1991, 1992; Entem & Machleidt 2003; Valderrama & Phillips 2015; Leutwyler 1994; Epelbaum et al. 2009; Otsuka et al. 2010; Holt et al. 2013; Hebeler et al. 2011; Drischler et al. 2014; Hebeler & Schwenk 2010; Carbone et al. 2013; Ekström et al. 2013; Coraggio et al. 2014).”