IONS STOPPING IN DENSE AND HOT MATTER

1983 ◽  
Vol 44 (C8) ◽  
pp. C8-67-C8-92 ◽  
Author(s):  
C. Deutsch ◽  
G. Maynard ◽  
H. Minoo
Keyword(s):  
Hot Matter

Strange and hot matter

1992 ◽  
Vol 544 (1-2) ◽  
pp. 279-292 ◽  
Author(s):  
Johann Rafelski
Keyword(s):  
Hot Matter

scholarly journals Atomic physics for beam-target interactions

1984 ◽  
Vol 2 (4) ◽  
pp. 449-465 ◽  
Author(s):  
C. Deutsch
Keyword(s):  
Electron Number Density ◽  
Accurate Determination ◽  
Projectile Energy ◽  
Stark Broadening ◽  
Number Density ◽  
Compact Formulation ◽  
Electron Contribution ◽  
Hot Matter ◽  
Special Relevance

This survey is devoted to a few basic atomic problems associated with the stopping of nonrelativistic pointlike ions in dense and hot matter, and also to the Stark broadening diagnostics of the resulting beam-produced plasmas.First, we consider the free electron contribution, taken in the RPA approximation with an exact dynamic dielectric function, valid at any temperature. Therefore, we obtain stopping power and straggling for any projectile velocity. The temperature dependence is of special relevance for a projectile energy smaller than 5 MeV/a.m.u.Next, we revise the Barkas effect (Z3 corrections) through a novel and compact formulation, which is based on an analogy with electron impact broadening theory. It facilitates inclusion of the non hydrogenic and electronic structure of the target ions, in a more selective way. The results may increase the usual Z2-stopping by 15 to 30 per cent corrections.Then, we show how the Stark broadening diagnostics of the compressed D + T fuel, seeded with high Z species, arising from the surrounding envelopes, may provide accurate determination of the electron number density ne. In this connection, it should be appreciated that the relatively long compression times (≃ 20 nsec) suggested by the HIBALL numerical simulation allow for a nearly Local Thermodynamic Equilibrium (LTE) state in the target, with Te ≃ Ti. As a consequence, spectroscopic measurements are expected to be easier to implement in HIF targets, than in laser ones.A tentative proposal for the use of Stark broadening diagnostics of inflight excited and highly stripped ion projectiles is displayed in § 5.Experiments involving an HIB produced by a standard accelerator, and interacting with an independently produced coronal plasma are finally outlined.

scholarly journals Impact of the Nuclear Equation of State on the Stability of Hybrid Neutron Stars

Universe ◽  
2019 ◽  
Vol 5 (8) ◽  
pp. 186 ◽  
Author(s):  
Mateusz Cierniak ◽  
Tobias Fischer ◽  
Niels-Uwe Bastian ◽  
Thomas Klähn ◽  
Marc Salinas
Keyword(s):  
Equations Of State ◽  
Mean Field Theory ◽  
Mean Field ◽  
Type Model ◽  
Two Phase ◽  
Relativistic Mean Field ◽  
Nuclear Equation Of State ◽  
Hot Matter ◽  
The Stability ◽  
Quark Phase

We construct a set of equations of state (EoS) of dense and hot matter with a 1st order phase transition from a hadronic system to a deconfined quark matter state. In this two-phase approach, hadrons are described using the relativistic mean field theory with different parametrisations and the deconfined quark phase is modeled using vBag, a bag–type model extended to include vector interactions as well as a simultaneous onset of chiral symmetry restoration and deconfinement. This feature results in a non–trivial connection between the hadron and quark EoS, modifying the quark phase beyond its onset density. We find that this unique property has an impact on the predicted hybrid (quark core) neutron star mass–radius relations.

Hadrons in dense and hot matter

2003 ◽  
Vol 18 (2-3) ◽  
pp. 453-458
Author(s):  
J. Wambach
Keyword(s):  
Hot Matter

Decay of ▭ in hot matter

1991 ◽  
Vol 262 (4) ◽  
pp. 485-491 ◽  
Author(s):  
Pin-Zhen Bi ◽  
Johann Rafelski
Keyword(s):  
Hot Matter

scholarly journals Neutrino Cooling of Primordial Hot Regions

Symmetry ◽  
2020 ◽  
Vol 12 (9) ◽  
pp. 1442
Author(s):  
Konstantin Belotsky ◽  
Mohamed El Kasmi ◽  
Sergey Rubin
Keyword(s):  
Symmetry Breaking ◽  
Lower Limit ◽  
Particle Concentration ◽  
Initial Temperature ◽  
Nuclear Reactions ◽  
Threshold Effect ◽  
Final Temperature ◽  
Hot Matter ◽  
Density Inhomogeneities

The effect of neutrino cooling of possible primary regions filled by hot matter is discussed. Such regions could be obtained from the primordial density inhomogeneities and survive up to the modern epoch. The inhomogeneities could be caused by a symmetry breaking during the inflationary stage. We show that the final temperature of such region should be ∼10 keV provided that the initial temperature is within the interval 10 keV ÷ 100 MeV. The cooling is realized due to the weak nuclear reactions containing n−p transition. The lower limit 10keV is accounted for by suppression of the reactions rates because of the threshold effect and particle concentration decrease.

scholarly journals Revisiting the hot matter in the center of gamma-ray bursts and supernovae

2013 ◽  
Vol 555 ◽  
pp. A129 ◽  
Author(s):  
Ang Li ◽  
Tong Liu
Keyword(s):  
Strong Interaction ◽  
Gamma Ray ◽  
Gamma Ray Bursts ◽  
Model Calculations ◽  
Hartree Fock ◽  
Equation Of States ◽  
Chemical Potentials ◽  
Hot Matter ◽  
Inner Region ◽  
Proto Neutron Star

Aims. Hot matter with nucleons can be produced in the inner region of the neutrino-dominated accretion flow in gamma-ray bursts or during the proto-neutron star birth in successful supernovae. The composition and equation of state of the matter depend on the dynamic β equilibrium under various neutrino opacities. The strong interaction between nucleons may also play an important role. We plan to extend the previous studies by incorporating these two aspects in our model. Methods. The modification of the β-equilibrium condition from neutrino optically thin to thick was modeled by an equilibrium factor χ ranging between the neutrino-freely-escaping case and the neutrino-trapped case. We employed the microscopic Brueckner-Hartree-Fock approach extended to the finite temperature regime to study the interacting nucleons. Results. We show the composition and chemical potentials of the hot nuclear matter for different densities and temperatures at each stage of β equilibrium. We also compare our realistic equation of states with those of the free-gas model. We find that it is important to properly describe the neutrino opacity and the strong interaction between nucleons, and they should be taken into account in model calculations.

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