@article {0253-6102-47-1-022,
	title = {Antikaon Condensation and In-medium Kaon and Antikaon Production in Protoneutron Stars},
	journal = {Communications in Theoretical Physics},
	volume = {47},
	number = {1},
	year = {2007},
	pages = {111},
	abstract = {Antikaon condensation and kaon and antikaon production in protoneutron stars are investigated in a chiral hadronic model (also referred to as the FST model in this paper). The effects of neutrino trapping on protoneutron stars are analyzed systematically. It is shown that neutrino trapping makes the critical density of K {\^a}{\textasciicircum}{\textquoteright} condensation delay to higher density and $\#$$\#$IMG$\#$$\#$ [http://ej.iop.org/icons/Entities/barK.gif] bar K 0 condensation not occur. The equation of state (EOS) of (proto)neutron star matter with neutrino trapping is stiffer than that without neutrino trapping. As a result, the maximum masses of (proto)neutron stars with neutrino trapping are larger than those without neutrino trapping. If hyperons are taken into account, antikaon does not form a condensate in (proto)neutron stars. Meanwhile, the corresponding EOS becomes much softer, and the maximum masses of (proto)neutron stars are smaller than those without hyprons. Finally, our results illustrate that the Q values for K + and K {\^a}{\textasciicircum}{\textquoteright} production in (proto)neutron stars are not sensitive to neutrino trapping and inclusion of hyperons.},
	url = {http://stacks.iop.org/0253-6102/47/i=1/a=022},
	author = {Gu Jian-Fa and Guo Hua and Li Xi-Guo and Liu Yu-Xin and Xu Fu-Rong}
}
