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arXiv 1002.1902nucl-thastro-ph.HEhep-phnucl-ex
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同位旋非对称核物质与轴对称中子星的性质

Isospin asymmetric nuclear matter and properties of axisymmetric neutron stars

Partha Roy Chowdhury, Abhijit Bhattacharyya, D. N. Basu

摘要:

利用DDM 3 Y有效相互作用得到的物态方程(EoS)可以得到引力质量超过极限值($\approx$ 1.6 M $_\odot$)的纯强子致密星,而大多数其它物态方程(EoS)的预测都局限于此。这种有效的相互作用被认为是相当成功的,在提供统一的描述弹性和非弹性散射,各种放射性和核物质的性质。本文系统地研究了纯强子致密星的性质。利用这个地壳薄的EoS,$β$平衡的中子星物质能够描述高质量的致密星,例如PSR B 1516 + 02 B的质量M=1.94 $^{+0.17}_{-0.19}$ M $_\odot$和PSR J 0751 +1807的质量M=2.1 $\pm$ 0.2 M $_\odot$,置信水平为1 $σ$。

英文摘要:

Pure hadronic compact stars, above a limiting value ($\approx$1.6 M$_\odot$) of their gravitational masses, to which predictions of most of other equations of state (EoSs) are restricted, can be reached from the equation of state (EoS) obtained using DDM3Y effective interaction. This effective interaction is found to be quite successful in providing unified description of elastic and inelastic scattering, various radioactivities and nuclear matter properties. We present a systematic study of the properties of pure hadronic compact stars. The $β$-equilibrated neutron star matter using this EoS with a thin crust is able to describe highly-massive compact stars, such as PSR B1516+02B with a mass M=1.94$^{+0.17}_{-0.19}$ M$_\odot$ and PSR J0751+1807 with a mass M=2.1$\pm$0.2 M$_\odot$ to a 1$σ$ confidence level.

机构、总结、中文摘要均由AI分析而来,可能存在错误,请以论文正文为准。

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