scholarly journals Boson Stars with Vector Meson Exchange Repulsive Interaction

2016 ◽  
Vol 739 ◽  
pp. 012075
Author(s):  
M Fitrah ◽  
Alfian Rangga Sakti ◽  
Anto Sulaksono
1968 ◽  
Vol 54 (4) ◽  
pp. 897-918 ◽  
Author(s):  
A. Bassetto ◽  
P. Campogalliani ◽  
F. Paccanoni

1993 ◽  
Vol 46 (6) ◽  
pp. 737
Author(s):  
GQ Liu ◽  
AW Thomas

To distinguish explicit quark effects from meson exchange in the NN interaction, it is necessary to splice the long-range meson exchange forces and short-distance dynamics due to quarks. However, in most quark model studies the short-range part of the pion exchange is usually treated differently, which makes it difficult to get a uniform picture of the short-range dynamics. We make a comparison between meson exchange and quark-gluon dynamics using the same pion exchange potential based on a quark-pion coupling model. The roles of vector meson exchange and gluon exchange in the NN interaction are compared by calculating NN phase parameters. It is shown that, with this consistent one-pion exchange force, the vector meson exchange gives a better fit to the data. This suggests that non-perturbative mechanisms responsible for meson exchange may need more careful handling to supplement the usual one-gluon exchange mechanism in describing the NN interaction.


1976 ◽  
Vol 14 (9) ◽  
pp. 2327-2339 ◽  
Author(s):  
H. Galic ◽  
B. Guberina ◽  
D. Tadić

1974 ◽  
Vol 53 ◽  
pp. 27-46
Author(s):  
H. A. Bethe

An equation of state is developed for densities from nuclear density (3 x 1014 g cm−3) to about 1016 g cm−3. The repulsive interaction between baryons dominates and empirical arguments for its existence are given. This interaction is attributed to vector meson exchange, and is derived from classical field theory whereupon a Yukawa potential results. The potential actually assumed is a modification of the Reid potential. Arguments are given that the baryons will not form a crystal lattice. The actual calculations were done using Pandharipande's method. The particles present at high density certainly include nucleons, Λ and Σ. The presence of Δ is questionable but that of π is likely. Results are given for the concentration of various species. With the more likely assumption about interactions, the concentration of each permissible species of particle is about equal at ϱ = 1016 g cm−3. The relation between energy and density is nearly independent of the assumptions on the species permitted and the energy is about 3 GeV particle−1 at ϱ = 1016 g cm−3. The relation between pressure and energy density is given, which yields a sound velocity equal to c at a few times 1015 g cm−3. Results for the structure of neutron stars are given. The maximum mass is about 2 solar masses and the maximum moment of inertia 1045 g cm2.


1983 ◽  
Vol 28 (6) ◽  
pp. 2423-2432 ◽  
Author(s):  
C. A. Gagliardi ◽  
G. T. Garvey ◽  
J. R. Wrobel ◽  
S. J. Freedman

2003 ◽  
Vol 729 (2-4) ◽  
pp. 743-768 ◽  
Author(s):  
J.E. Palomar ◽  
L. Roca ◽  
E. Oset ◽  
M.J. Vicente Vacas

1978 ◽  
Vol 17 (1) ◽  
pp. 174-184 ◽  
Author(s):  
M. G. Olsson ◽  
E. T. Osypowski

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