High Density Equations of State and the Inner Structure of Neutron Stars. Theory Versus Observations.

Details High Density Equations of State and the Inner Structure of Neutron Stars. Theory Versus Observations. High Density Equations of State and the Inner Structure of Neutron Stars. Theory Versus Observations.

Sep 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001cnoc.conf...13d&link_type=abstract

The Second National Conference on Astrophysics of Compact Objects, held in Bologna (Italy), September 19 - 21, 2001, p. 13

Astronomy and Astrophysics

Astrophysics

Scientific paper

I will review the main problems concerning the equation of state of matter at high density. In particular I will discuss the possible transition to a phase of deconfined quarks. The deconfinement transition, if it takes place inside neutron stars, affects many observables, such as the radius of the star, its cooling curve and also the stability of the star itself. I will try to stress the possible signatures in astrophysical observations of the various theoretical possibilities concerning the inner composition of a neutron star.

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