We have studied the effect of tidal deformability constraint given by the binary neutron star merger event GW170817 on the equations of state (EOS) of hybrid stars. The EOS are constructed by matching the hadronic EOS described by relativistic mean field (RMF) model and parameter sets NL3, TM1 and NL3ωρ with the quark matter EOS described by modified MIT bag model, viaGibbs' construction. It is found that the tidal deformability constraint along with the lower bound on maximum mass (M max = 2.01±0.04M ⊙ ) significantly limits the bag model parameter space (B 1/4 eff , a 4 ). We also obtain upper limits on the radius of 1.4M ⊙ and 1.6M ⊙ stars as R 1.4 ≤ 13.2 − 13.5 km and R 1.6 ≤ 13.2 − 13.4 km, respectively for different hadronic EOS considered here.
We show that the odds of the mass-gap (secondary) object in GW190814 being a neutron star (NS) improve if one allows for a stiff high-density equation of state (EoS) or a large spin. Since its mass is ∈ (2.50, 2.67) M⊙, establishing its true nature will make it either the heaviest NS or the lightest black hole (BH), and can have far-reaching implications on NS EoS and compact object formation channels. When limiting oneself to the NS hypothesis, we deduce the secondary’s properties by using a Bayesian framework with a hybrid EoS formulation that employs a parabolic expansion-based nuclear empirical parameterization around the nuclear saturation density augmented by a generic 3-segment piecewise polytrope (PP) model at higher densities and combining a variety of astrophysical observations. For the slow-rotation scenario, GW190814 implies a very stiff EoS and a stringent constraint on the EoS specially in the high-density region. On the other hand assuming the secondary object is a rapidly rotating NS, we constrain its rotational frequency to be $f=1170^{+389}_{-495}$ Hz, within a $90{{\ \rm per\ cent}}$ confidence interval (CI). In this scenario, the secondary object in GW190814 would qualify as the fastest rotating NS ever observed. However, for this scenario to be viable, rotational instabilities would have to be suppressed both during formation and the subsequent evolution until merger, otherwise the secondary of GW190814 is more likely to be a BH.
Radio frequency, microwave, and infrared spectra have been obtained from molecular beams of acetylene dimer. The geometry of the isomer studied here is T shaped, with the centers of mass of the monomers separated by 4.38 A. The equilibrium structure appears not to have C 2v symmetry and the vibrationally averaged structure has the "top" of the T rotated about its center of mass by 27·. The electric dipole moment of this complex is 0.28 D.
In the late inspiral phase, gravitational waves from binary neutron star mergers carry the imprint of the equation of state due to the tidally deformed structure of the components. If the stars contain solid crusts, then their shear modulus can affect the deformability of the star and, thereby, modify the emitted signal. Here, we investigate the effect of realistic equations of state (EOSs) of the crustal matter, with a realistic model for the shear modulus of the stellar crust in a fully general relativistic framework. This allows us to systematically study the deviations that are expected from fluid models. In particular, we use unified EOSs, both relativistic and non-relativistic, in our calculations. We find that realistic EOSs of crusts cause a small correction, of ∼ 1%, in the second Love number. This correction will likely be subdominant to the statistical error expected in LIGO-Virgo observations at their respective advanced design sensitivities, but rival that error in third generation detectors. For completeness, we also study the effect of crustal shear on the magnetic-type Love number and find it to be much smaller.
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