Abstract
The transition from a neutron star to a pion-condensed star is investigated in Newtonian hydrodynamics. It is shown that in a certain range of ultradense equations of state, there occurs a mass ejection with energies comparable with usual supernova outputs. But the ejected mass is only in the order of 0.02M ⊙.
Therefore, the observable consequences of this transition are not so dramatic as conjectured recently. In a realistic scenario including a stiff ultradense equation of state and a weak effect of pion condensation the mass ejection disappears.
Additionally the collapse of a stellar core to a neutron star with pion-condensed core is considered. In comparison with a standard supernova scenario we find only a slightly reduced explosion energy.
Further, the possible consequence of pion condensation during the secular evolution of the bounced core of a collapsing star to the cool final neutron star is discussed.
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Kämpfer, B. On the collapse of neutron stars and stellar cores to pion-condensed stars. Astrophys Space Sci 93, 185–197 (1983). https://doi.org/10.1007/BF02430922
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DOI: https://doi.org/10.1007/BF02430922