Send to

Choose Destination
Phys Rev Lett. 2016 Jul 15;117(3):032501. doi: 10.1103/PhysRevLett.117.032501. Epub 2016 Jul 12.

Holographic Quark Matter and Neutron Stars.

Author information

Department of Physics, Universidad de Oviedo, Avenida Calvo Sotelo 18, ES-33007 Oviedo, Spain.
Department of Physics and Helsinki Institute of Physics, University of Helsinki, P.O. Box 64, Helsinki FI-00014, Finland.


We use a top-down holographic model for strongly interacting quark matter to study the properties of neutron stars. When the corresponding equation of state (EOS) is matched with state-of-the-art results for dense nuclear matter, we consistently observe a first-order phase transition at densities between 2 and 7 times the nuclear saturation density. Solving the Tolman-Oppenheimer-Volkov equations with the resulting hybrid EOSs, we find maximal stellar masses in excess of two solar masses, albeit somewhat smaller than those obtained with simple extrapolations of the nuclear matter EOSs. Our calculation predicts that no quark matter exists inside neutron stars.

Supplemental Content

Full text links

Icon for American Physical Society
Loading ...
Support Center