| Popis: |
We show that certain classical solutions of hadronic effective field theories can model neutron stars. Within the uncertainties of what is known from laboratory measurements of nuclear physics, these solutions, called Q-stars, may have masses much larger (⪢ 3 M ⊙) or may be able to rotate faster (Prot < 0.5 ms) than previously believed possible. Stable chunks of nuclear density baryonic matter varying in size from 10−12 cm to several kilometers may also exist. Cygnus X-1, LMC X-3, and the SN1987A remnant are candidates for Q-stars. |
