Direct URCA Process in Neutron Stars

SHEN Gang; MENG Jie; Hillhouse G

Chinese Physics C> 2004, Vol. 28> Issue(S1) : 99-101

Direct URCA Process in Neutron Stars

School of Physics, Peking University, Beijing 100871, China2 Institute of Theoretical Physics, Chinese Academy of Sciences, Beijing 100871, China3 Center of Theoretical Nuclear Physics, National Laboratory of Heavey Ion Accelerator, Lanzhou 730000, China4 Department of Physics, University of Stellenbosch, Stellenbosch, South Africa

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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.

References

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SHEN Gang, MENG Jie and Hillhouse G. Direct URCA Process in Neutron Stars[J]. Chinese Physics C, 2004, 28(S1): 99-101.

SHEN Gang, MENG Jie and Hillhouse G. Direct URCA Process in Neutron Stars[J]. Chinese Physics C, 2004, 28(S1): 99-101. shu

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Received: 2004-12-30
Revised: 1900-01-01

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沈阳化工大学材料科学与工程学院沈阳 110142

Direct URCA Process in Neutron Stars

Corresponding author: MENG Jie,

School of Physics, Peking University, Beijing 100871, China2 Institute of Theoretical Physics, Chinese Academy of Sciences, Beijing 100871, China3 Center of Theoretical Nuclear Physics, National Laboratory of Heavey Ion Accelerator, Lanzhou 730000, China4 Department of Physics, University of Stellenbosch, Stellenbosch, South Africa

Received Date: 2004-12-30
Accepted Date: 1900-01-01
Available Online: 2004-04-02

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.