H-1 - Neutron-star matter has a stiff equation of state - no hyperons, bosons, or free quarks near nuclear saturation density
Properties9
type
hypothesis
id
H-1
state
active
question
What is the equation of state of cold matter at supranuclear densities?
statement
The equation of state of cold matter at supranuclear densities is stiff enough to support neutron stars of at least 1.97 Msun; EOS models that soften through the appearance of exotic hadronic matter (hyperons, kaon condensates) or free quarks at a few times nuclear saturation density are not realized in neutron-star interiors (condensed quark matter is not fully excluded but is strongly constrained).
The EOSs which produce the lowest maximum masses tend to be those which predict significant softening past a certain central density. ... All such EOSs are ruled out by our results.