Constraining URCA cooling of neutron stars from the neutron radius of 208Pb

C. J. Horowitz, J. Piekarewicz

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164 Scopus citations

Abstract

Recent observations by the Chandra observatory suggest that some neutron stars may cool rapidly, perhaps by the direct URCA process which requires a high proton fraction. The proton fraction is determined by the nuclear symmetry energy whose density dependence may be constrained by measuring the neutron radius of a heavy nucleus, such as 208Pb. Such a measurement is necessary for a reliable extrapolation of the proton fraction to the higher densities present in a neutron star. A large neutron radius in 208Pb implies a stiff symmetry energy that grows rapidly with density, thereby favoring a high proton fraction and allowing direct URCA cooling. Predictions for the neutron radius in 208Pb are correlated to the proton fraction in dense matter by using a variety of relativistic effective field-theory models. Models that predict a neutron (Rn) minus proton (Rp) root-mean-square radius in 208Pb to be Rn-Rp≲0.20 fm have proton fractions too small to allow the direct URCA cooling of 1.4A neutron stars. Conversely, if Rn-Rp≳0.25 fm, the direct URCA process is allowed (by all models) to cool down a 1.4M neutron star. The Parity Radius Experiment at Jefferson Laboratory aims to measure the neutron radius in 208Pb accurately and model independently via parity-violating electron scattering. Such a measurement would greatly enhance our ability to either confirm or dismiss the direct URCA cooling of neutron stars.

Original languageEnglish
Article number055803
Pages (from-to)558031-5580335
Number of pages5022305
JournalPhysical Review C - Nuclear Physics
Volume66
Issue number5
StatePublished - 1 Nov 2002
Externally publishedYes

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