scholarly journals Influence of the equation of state of matter and ion beam characteristics on target heating and compression

2003 ◽  
Vol 6 (2) ◽  
Author(s):  
N. A. Tahir ◽  
A. Shutov ◽  
D. Varentsov ◽  
P. Spiller ◽  
S. Udrea ◽  
...  
Keyword(s):  
Equation Of State ◽  
Ion Beam ◽  
State Of Matter ◽  
Beam Characteristics

High-Power Ion Beam Characteristics of a Magnetic Multi-Pole Line-Cusp Ion Source for the HL-2A Tokomak

2009 ◽  
Vol 26 (8) ◽  
pp. 082901 ◽  
Author(s):  
Zou Gui-Qing ◽  
Lei Guang-Jiu ◽  
Jiang Shao-Feng ◽  
Cao Jian-Yong ◽  
Yu Li-Ming ◽  
...  
Keyword(s):  
High Power ◽  
Ion Beam ◽  
Ion Source ◽  
Beam Characteristics

scholarly journals Plasma Acceleration and Heating Using Hybrid Magnetic Fields

2008 ◽  
Vol 63 (7-8) ◽  
pp. 419-422
Author(s):  
Alexandre Pozwolski
Keyword(s):  
Magnetic Field ◽  
Equation Of State ◽  
Constant Magnetic Field ◽  
Axial Velocity ◽  
Repulsive Force ◽  
Plasma Acceleration ◽  
Fusion Reactions ◽  
High Concentration ◽  
Laboratory Equipment ◽  
State Of Matter

The repulsive force between two wires with large currents flowing in opposite directions through the wires can be used to propel a light circular conductor located above a massive ring. Then the axial velocity can reach 500 km/s and an auxiliary constant magnetic field controls the radial velocity. This allows to get a high concentration of energy at any distance from the laboratory equipment. A further application could be the investigation of the equation of state of matter at high densities and the triggering of fusion reactions.

scholarly journals Fundamental physics and the absence of sub-millisecond pulsars

2018 ◽  
Vol 620 ◽  
pp. A69 ◽  
Author(s):  
B. Haskell ◽  
J. L. Zdunik ◽  
M. Fortin ◽  
M. Bejger ◽  
R. Wijnands ◽  
...  
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Neutron Stars ◽  
Gravitational Wave ◽  
Equations Of State ◽  
Rotation Frequency ◽  
Hadronic Matter ◽  
Spin Distribution ◽  
Test Models ◽  
State Of Matter

Context. Rapidly rotating neutron stars are an ideal laboratory to test models of matter at high densities. In particular, the maximum rotation frequency of a neutron star depends on the equation of state and can be used to test models of the interior. However, observations of the spin distribution of rapidly rotating neutron stars show evidence for a lack of stars spinning at frequencies higher than f ≈ 700 Hz, well below the predictions of theoretical equations of state. This has generally been taken as evidence of an additional spin-down torque operating in these systems, and it has been suggested that gravitational wave torques may be operating and be linked to a potentially observable signal. Aims. We aim to determine whether additional spin-down torques (possibly due to gravitational wave emission) are necessary, or if the observed limit of f ≈ 700 Hz could correspond to the Keplerian (mass-shedding) break-up frequency for the observed systems, and is simply a consequence of the currently unknown state of matter at high densities. Methods. Given our ignorance with regard to the true equation of state of matter above nuclear saturation densities, we make a minimal physical assumption and only demand causality, that is, that the speed of sound in the interior of the neutron star should be lower than or equal to the speed of light c. We then connected our causally limited equation of state to a realistic microphysical crustal equation of state for densities below nuclear saturation density. This produced a limiting model that gave the lowest possible maximum frequency, which we compared to observational constraints on neutron star masses and frequencies. We also compared our findings with the constraints on the tidal deformability obtained in the observations of the GW170817 event. Results. We rule out centrifugal breakup as the mechanism preventing pulsars from spinning faster than f ≈ 700 Hz, as the lowest breakup frequency allowed by our causal equation of state is f ≈ 1200 Hz. A low-frequency cutoff, around f ≈ 800 Hz could only be possible when we assume that these systems do not contain neutron stars with masses above M ≈ 2 M⊙. This would have to be due either to selection effects, or possibly to a phase transition in the interior of the neutron star that leads to softening at high densities and a collapse to either a black hole or a hybrid star above M ≈ 2 M⊙. Such a scenario would, however, require a somewhat unrealistically stiff equation of state for hadronic matter, in tension with recent constraints obtained from gravitational wave observations of a neutron star merger.

A General equation of state of matter

1978 ◽  
Vol 21 (11) ◽  
pp. 405-408 ◽  
Author(s):  
F. Mulargia
Keyword(s):  
Equation Of State ◽  
General Equation ◽  
State Of Matter

Plasma and Ion Beam Characteristics of the Dynamag Ion Source

1962 ◽  
Vol 33 (12) ◽  
pp. 1338-1339 ◽  
Author(s):  
Edwin M. Kellogg ◽  
Karl E. Eklund
Keyword(s):  
Ion Beam ◽  
Ion Source ◽  
Beam Characteristics

Magnetic field configurations on thruster performance in accordance with ion beam characteristics in cylindrical Hall thruster plasmas

2017 ◽  
Vol 110 (11) ◽  
pp. 114101 ◽  
Author(s):  
Holak Kim ◽  
Wonho Choe ◽  
Youbong Lim ◽  
Seunghun Lee ◽  
Sanghoo Park
Keyword(s):  
Magnetic Field ◽  
Ion Beam ◽  
Hall Thruster ◽  
Beam Characteristics

scholarly journals The State of Matter in Simulations of Core-Collapse supernovae—Reflections and Recent Developments

2017 ◽  
Vol 34 ◽  
Author(s):  
Tobias Fischer ◽  
Niels-Uwe Bastian ◽  
David Blaschke ◽  
Mateusz Cierniak ◽  
Matthias Hempel ◽  
...  
Keyword(s):  
Equation Of State ◽  
Degrees Of Freedom ◽  
The State ◽  
Core Collapse ◽  
Heavy Nuclei ◽  
Isospin Asymmetry ◽  
Wide Range ◽  
Recent Developments ◽  
State Of Matter

AbstractIn this review article, we discuss selected developments regarding the role of the equation of state in simulations of core-collapse supernovae. There are no first-principle calculations of the state of matter under supernova conditions since a wide range of conditions is covered, in terms of density, temperature, and isospin asymmetry. Instead, model equation of state are commonly employed in supernova studies. These can be divided into regimes with intrinsically different degrees of freedom: heavy nuclei at low temperatures, inhomogeneous nuclear matter where light and heavy nuclei coexist together with unbound nucleons, and the transition to homogeneous matter at high densities and temperatures. In this article, we discuss each of these phases with particular view on their role in supernova simulations.

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