Jan 26 – 30, 2015
Bormio, Italy
Europe/Berlin timezone

The Neutron Star Mass-Radius Relationship and the Dense Matter Equation of State

Jan 26, 2015, 9:10 AM
Bormio, Italy

Bormio, Italy

Overview Talk Nuclear Structure and Astrophysics Monday Morning


Prof. Robert Rutledge


Neutron stars -- the densest objects in the universe -- are supported against gravitational collapse by pressure arising from the dense matter equation of state (dEOS) -- the pressure as a function of density, at and above nuclear densities. The dEOS arises from fundamental interactions, and so is of fundamental interest -- in much the same way that the ideal gas law was of interest arising from atomic gas theory at the dawn of thermodynamics; yet predicting the dEOS is fraught with uncertainty in the physics, as well as in the calculational approximations necessary to undertake what would otherwise be intractable. But, with a dEOS specified, the mass-radius relationship for neutron stars can be easily calculated; inversely, in the absence of a dEOS, measurements of the neutron star mass-radius relationship constrain the dEOS. I will review astrophysical observational results, from X-ray spectroscopy of neutron stars, and point toward how these results can be used to infer the form of the dEOS.

Primary author

Prof. Robert Rutledge (McGill University)

Presentation materials