Condensed<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:msup><mml:mrow><mml:mi>π</mml:mi></mml:mrow><mml:mrow><mml:mo>−</mml:mo></mml:mrow></mml:msup></mml:mrow></mml:math>Phase in Neutron-Star Matter

It is argued that at some density, estimated at about 1 baryon/${\mathrm{F}}^{3}$, superdense nuclear matter will make a transition to a phase of approximately equal numbers of protons, neutrons, and ${\ensuremath{\pi}}^{\ensuremath{-}}$ particles, the latter condensed in one or two plane-wave states of momentum $\ensuremath{\approx}170 \frac{\mathrm{MeV}}{c}$. These conclusions are based on the conventional theory of the pionnucleon interaction.

Hali tarjima qilinmagan