Microscopic calculation of the equation of state of nuclear matter and neutron star structure

被引：64

作者：

Gandolfi, S. ^{[1
,2
,3
]}

Illarionov, A. Yu. ^{[2
,3
,4
]}

Fantoni, S. ^{[2
,3
,5
]}

Miller, J. C. ^{[2
,3
,6
]}

Pederiva, F. ^{[4
,7
]}

Schmidt, K. E. ^{[8
]}

机构：

[1] Los Alamos Natl Lab, Div Theoret, Los Alamos, NM 87545 USA

[2] SISSA, Int Sch Adv Studies, I-34014 Trieste, Italy

[3] Ist Nazl Fis Nucl, Sez Trieste, Trieste, Italy

[4] Univ Trento, Dipartimento Fis, I-38123 Povo, Trento, Italy

[5] INFM, DEMOCRITOS Natl Simulat Ctr, I-34014 Trieste, Italy

[6] Univ Oxford, Dept Phys Astrophys, Oxford OX1 3RH, England

[7] Ist Nazl Fis Nucl, Grp Collegato Trento, Trento, Italy

[8] Arizona State Univ, Dept Phys, Tempe, AZ 85287 USA

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2010年 / 404卷 / 01期

基金：

美国国家科学基金会;

关键词：

equation of state; stars: neutron;

D O I：

10.1111/j.1745-3933.2010.00829.x

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present results for neutron star models constructed with a new equation of state for nuclear matter at zero temperature. The ground state is computed using the auxiliary field diffusion Monte Carlo (AFDMC) technique, with nucleons interacting via a semiphenomenological Hamiltonian including a realistic two-body interaction. The effect of many-body forces is included by means of additional density-dependent terms in the Hamiltonian. In this Letter, we compare the properties of the resulting neutron star models with those obtained using other nuclear Hamiltonians, focusing on the relations between mass and radius, and between the gravitational mass and the baryon number.

引用

页码：L35 / L39

页数：5

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