Erratum: Role of higher order couplings in the presence of kaons in relativistic mean field description of neutron stars [Phys. Rev. C85, 015804 (2012)]

Abstract

FIG. 9. (Color online) The mass-radius relation for nonkaonic and kaonic phases using different parameter sets. The calculations done without considering kaons are represented by the small dotted lines. The solid circles represent the maximum mass in every case. Mass is given in units of solar mass M . Solid squares (r ph = R) and open triangles (r ph R) represent the observational constraints [1], where r ph is the photospheric radius. The shaded region corresponds to the recent observation of a 1.97 ± 0.04M star [6].[1] A.

On the Maximum Mass of Neutron Stars

“…Still, some RMF models including kaon condensates are able to predict the existence of massive NSs with M > 2 M . 61 Consistency of the kaon condensation model with 2 M pulsar necessitates, however, a tuning of the parameters of the RMF model.…”

Phase transitions in dense matter and the maximum mass of neutron stars

“…This discrepancy can be understood at least partly from the fact that the maximum mass is A&A 553, A22 (2013) very sensitive to the various hyperonic couplings, and these are determined very poorly since the limited nuclear and hypernuclear data that are relevant constrain the EoS only in the vicinity of the saturation density, whereas the maximum neutron-star mass is mostly determined by the EoS at much higher densities. Likewise, some relativistic mean-field models including meson condensates are able to predict the existence of massive neutron stars (Gupta & Arumugam 2012).…”

Neutron Stars With Kaon Condensation in Relativistic Effective Model

“…We should emphasize that in Ref. 28 the authors calculate the neutron stars with kaon condensate systematically by using lot of RMF models including the FSUGold model. In our paper, we calculate not only the FSUGold model but also the IU-FSU model with different values of U K .…”

“…In fact, the inner cores of the neutron stars are sources of speculation, some of the possibilities being the appearance of hyperons, 2-4 only quarks, [5][6][7][8][9][10] or Kaon condensates. [11][12][13][14][15][16][17][18][19][20][21][22][23][24][25][26][27][28] In this work, we will investigate the role of strangeness by introducing Kaon condensation in the neutron star matter.…”

“…In Ref. 28, the authors study the role of higher-order couplings of RMF models on the onset and effect of kaon condensation in neutron stars, they calculate the neutron star properties with the successful RMF parameters NL1 and NL3, the E-RMF parameters G1 and G2 and the FSUGold parameters. In this paper, we will give numerical results of the FSUGold model and the IU-FSU model with different values of U K , and discuss the main comparison between the extension of the two models with Kaon condensation.…”