Zobrazeno 1 - 10
of 83
pro vyhledávání: '"De-Hua Wen"'
Publikováno v:
The European Physical Journal A. 57
Based on the distribution of tidal deformabilities and component masses of binary neutron star merger GW170817, the parametric equation of states (EOS) are employed to probe the nuclear symmetry energy and the properties of neutron star. To obtain a
Publikováno v:
Progress of Theoretical and Experimental Physics. 2020
As some neutron star transients require an additional unknown heat source (referred to as “shallow heating”) to explain their high temperatures at the beginning of quiescence, we investigate the effect of shallow heating as well as compressional
Publikováno v:
Communications in Theoretical Physics. 73:115302
Due to improvements in the sensitivity of gravitational wave (GW) detectors, the detection of GWs originating from the fundamental quasi-normal mode (f-mode) of neutron stars has become possible. The future detection of GWs originating from the f-mod
Determining the Equation of State (EOS) of dense neutron-rich nuclear matter is a shared goal of both nuclear physics and astrophysics. Except possible phase transitions, the density dependence of nuclear symmetry \esym is the most uncertain part of
Externí odkaz:
https://explore.openaire.eu/search/publication?articleId=doi_dedup___::c8e6d9221d7916d20c49c3a8d881724e
http://arxiv.org/abs/1905.13175
http://arxiv.org/abs/1905.13175
Publikováno v:
Physical Review C. 99
Within a minimum model for neutron stars consisting of nucleons, electrons and muons at $\beta$-equilibrium using about a dozen Equation of States (EOSs) from microscopic nuclear many-body theories and 40,000 EOSs randomly generated using an explicit
Publikováno v:
Physical Review C. 99
Internal structure and macroscopic properties of neutron stars are strongly correlated with the equation of state (EOS) of dense matter, while the EOS remains exceedingly uncertain especially at high densities. The observed massive neutron star with
Inasmuch as the hydrostatic structure of interior neutron stars uniquely depends on the equation of state (EOS), the inverse constraints on EOS from astrophysical observation have been important methods to reveal the properties of the high-density ma
Externí odkaz:
https://explore.openaire.eu/search/publication?articleId=doi_dedup___::cbb8dc7989f5021bbc495db381c01696
http://arxiv.org/abs/1903.04875
http://arxiv.org/abs/1903.04875
Publikováno v:
AIP Conference Proceedings.
The density dependence of nuclear symmetry energy is the most uncertain part of the Equation of Sate (EOS) of neutron-rich nucleonic matter at supra-saturation densities. To pin down the latter has been a longstanding and shared goal of both nuclear
Similar to the compactness parameter ($\beta=M/R$), the gravitational binding energy (GBE) is also a characteristic parameter which can reflect the internal structure of a neutron star and thus can be used to expressing the universal relations. Scali
Externí odkaz:
https://explore.openaire.eu/search/publication?articleId=doi_dedup___::43809d225df9ed6e116ee75d8808c0b9
Autor:
Yong-Mei Wen, De-Hua Wen
Publikováno v:
Physical Review C. 95
By employing four typical equation of states (EOSs) of nuclear matter in the inner crust, the properties of low-mass neutron stars are investigated theoretically. Based on the well-known fact that there is a big gap between the neutron stars and whit