Neutron skins and neutron stars
نویسندگان
چکیده
منابع مشابه
Proto-neutron and Neutron Stars
It has been shown that effective chiral hadronic models can satisfactorily describe nuclear matter, properties of finite nuclei as well as the structure of neutron stars1. While most of the approaches are based on variations of the linear sigma model or its non-linear realization, in the approach discussed here the scalar sigma meson serves to split the nucleon and its chiral partner (particle ...
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In the present work, we have obtained the equation of state for neutron star matter considering the in uence of the ferromagnetic and antiferromagnetic spin state. We have also investigated the structure of neutron stars. According to our results, the spin asymmetry stiens the equation of state and leads to high mass for the neutron star.
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9 Black holes and neutron stars are fascinating objects with great potential for testing physical theories in extreme conditions. The gravitational fields near these objects provide an opportunity for tests of General Relativity in the strong-field limit and the properties of matter at the remarkably high densities that exist within neutron stars are unknown. While many of these objects are in ...
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in the present work, we have obtained the equation of state for neutron star matter considering the in uence of the ferromagnetic and antiferromagnetic spin state. we have also investigated the structure of neutron stars. according to our results, the spin asymmetry sti ens the equation of state and leads to high mass for the neutron star.
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We present here the results of Arecibo timing of PSR B1516+02B, a 7.95-ms pulsar in a binary system with a ∼ 0.17M⊙ companion and an orbital period of 6.85 days located in the globular cluster M5. The eccentricity of the orbit (e = 0.14) has allowed a measurement of the rate of advance of periastron: ω̇ = (0.0136 ± 0.0007)◦yr−1. It is very likely that the periastron advance is due to the effects...
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ژورنال
عنوان ژورنال: Physical Review C
سال: 2012
ISSN: 0556-2813,1089-490X
DOI: 10.1103/physrevc.86.015802