Observational implications of a strong phase transition in the dense matter equation of state for the rotational evolution of neutron stars
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M. Bejger | P. Haensel | D. Blaschke | J. Zdunik | M. Fortin
[1] I. Karpenko,et al. Event simulation based on three-fluid hydrodynamics for collisions at energies available at the Dubna Nuclotron-based Ion Collider Facility and at the Facility for Antiproton and Ion Research in Darmstadt , 2016, 1608.00965.
[2] S. Bogdanov,et al. THE IMPACT OF SURFACE TEMPERATURE INHOMOGENEITIES ON QUIESCENT NEUTRON STAR RADIUS MEASUREMENTS , 2016, 1605.09400.
[3] M. Bejger,et al. Neutron star radii and crusts: Uncertainties and unified equations of state , 2016, 1604.01944.
[4] Zaven Arzoumanian,et al. THE NANOGRAV NINE-YEAR DATA SET: MASS AND GEOMETRIC MEASUREMENTS OF BINARY MILLISECOND PULSARS , 2016, 1603.00545.
[5] Garching,et al. Inferring neutron-star properties from gravitational-wave signals of binary mergers , 2015, 1503.08769.
[6] A. Schwope,et al. The Hot and Energetic Universe: End points of stellar evolution , 2013, 1306.2334.
[7] D. Alvarez-Castillo,et al. Proving the CEP with compact stars , 2013, 1304.7758.