High density with elliptic flows

Trautmann, W.

doi:10.1063/1.5117793

Cited by 8 publications

(3 citation statements)

References 108 publications

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“…Understanding the nature and constraining the equation of state (EOS) of asymmetric nuclear matter have jointly been a major science goal shared by many astrophysical observations and nuclear experiments [1][2][3][4][5][6][7][8]. They also drive the construction of many radioactive beam facilities [9][10][11][12][13][14][15], X-ray observatories, and gravitational wave detectors [16][17][18][19][20][21] around the world. A basic input in calculating the EOS of nuclear matter is the specific energy , with ρ representing the nucleon density and being the isospin asymmetry, where and are the densities of neutrons and protons, respectively.…”

Section: Introductionmentioning

confidence: 99%

Dependence of the tidal deformability of neutron stars on the nuclear equation of state*

Wang

Chen²,

Ma³

et al. 2023

Chinese Phys. C

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Within the Bayesian framework using an explicitly isospin-dependent parametric equation of state (EOS) for the core of neutron stars (NSs), we study how the NS EOS behave when we confront them with the tidal deformabilities $\Lambda_{1.4}$ of canonical NSs with different error and different lower boundaries, and with the tidal deformabilities of the massive NSs. We found that it will not highly improve the constraints on the NS EOS but have a weak effect on narrowing down the slope parameter of the symmetry energy by decreasing the measurement errors of $\Lambda_{1.4}$. Both the isospin-dependent and isospin-independent parts of the NS EOS are significantly constrained and raised as the tidal deformabilities of the massive NSs are adopted in the calculations, especially in high-density regions. It is also found that $\Lambda_{1.4}$ is more competent to limit the curvature parameter than the slope parameter of the symmetry energy, whereas the opposite case happens for the radius of canonical NSs $R_{1.4}$. The tidal deformability of the NS with two times of solar mass $\Lambda_{2.0}$ is more sensitive to the skewness than curvature parameter of the symmetry energy, and $\Lambda_{1.4}$ and $R_{1.4}$ have no correlation with the former.

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Section: Introductionmentioning

confidence: 99%

Dependence of the tidal deformability of neutron stars on the nuclear equation of state*

Wang

Chen²,

Ma³

et al. 2023

Chinese Phys. C

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“…The point at the top of Fig. 18 has been obtained in [222] by converting the symmetry energy slope parameter range from the ASY-EOS heavy-ion experiment [36] to the NS radius range, using the known tight correlation between the symmetry pressure p 0 and the radius R 1.4 of a canonical neutron star of 1.4 M [229]. The corresponding R N S value amounts to 12.65 ± 0.75 km .…”

Section: Connection Of Asy-eos Results With Multi-messenger Astrophys...mentioning

confidence: 99%

“…The data point for J0437 MSP measured by HST+ROSAT (green filled square) was taken from [211]. The radius range labeled as ASY-EOS was obtained by translating the symmetry energy slope parameter range obtained from the ASY-EOS heavy-ion experiment [36] to the NS radius range [222]. It corresponds to a NS mass of 1.4 M but has been displaced arbitrarily in vertical direction for clarity.…”

Section: Shenmentioning

confidence: 99%

Studies of the equation-of-state of nuclear matter by heavy-ion collisions at intermediate energy in the multi-messenger era

Russotto¹,

Cozma²,

Filippo³

et al. 2023

Preprint

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The study of the nuclear matter equation-of-state (EoS) is a relevant topic of modern nuclear physics. It governs the behaviour of nuclear matter away from the normal conditions found in nuclei interiors and plays a major role in heavy-ion collisions, in determining neutron skin thicknesses of neutron rich nuclei and the mass-radius relation of neutron stars, and in modelizations of supernovae explosions. Its uncertain knowledge is related to difficulties in solving the many-body problem with realistic nuclear interactions. In the last decades several studies, from both theoretical and experimental sides, have allowed relevant progress in the description of the EoS, both for the isospin-symmetric matter and for the isospin-asymmetric matter, the so called symmetry energy, especially at densities below the saturation point. In this paper we review some of the studies on the high-density behavior of the EoS, obtained by studying heavy-ion collisions with incident energies between several hundred MeV up to about 2 GeV per nucleon, with a focus on those carried out at the GSI laboratory in Darmstadt (Germany) by using the SIS18 accelerator beams. Constraints on the isospin-symmetric matter

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Studies of the equation-of-state of nuclear matter by heavy-ion collisions at intermediate energy in the multi-messenger era

et al. 2023

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High density with elliptic flows

Cited by 8 publications

References 108 publications

Dependence of the tidal deformability of neutron stars on the nuclear equation of state*

Dependence of the tidal deformability of neutron stars on the nuclear equation of state*

Studies of the equation-of-state of nuclear matter by heavy-ion collisions at intermediate energy in the multi-messenger era

Studies of the equation-of-state of nuclear matter by heavy-ion collisions at intermediate energy in the multi-messenger era

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