Direct URCA process in neutron stars

Gang Shen, Jie Meng, G. C. Hillhouse

Research output: Contribution to journalArticle

Abstract

The onset of the most powerful neutrino emission candidate in the cooling of neutron stars, direct URCA process, requires a high threshold proton fraction. The proton fraction in neutron stars relies on the isospin dependent part of nuclear force, which can be constrained by the measurement of the neutron skin thickness in heavy nuclei such as 208Pb. Adding new isospin dependent correction terms to the effective interactions PK1, NL3, S271 and Z271, the correlation between the proton fraction and neutron skin thickness in 208Pb is studied. For a neutron star with fixed mass, the central proton fraction increases with increasing predicted values of neutron skin thickness in 208Pb.

Original languageEnglish
Pages (from-to)99-101
Number of pages3
JournalKao Neng Wu Li Yu Ho Wu Li/High Energy Physics and Nuclear Physics
Volume28
Issue numberSUPPL.
Publication statusPublished - Dec 1 2004

Fingerprint

neutron stars
protons
neutrons
heavy nuclei
neutrinos
cooling
thresholds
interactions

All Science Journal Classification (ASJC) codes

  • Nuclear and High Energy Physics
  • Physics and Astronomy(all)

Cite this

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Direct URCA process in neutron stars. / Shen, Gang; Meng, Jie; Hillhouse, G. C.

In: Kao Neng Wu Li Yu Ho Wu Li/High Energy Physics and Nuclear Physics, Vol. 28, No. SUPPL., 01.12.2004, p. 99-101.

Research output: Contribution to journalArticle

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