Effects of clustering in the equation of state for neutron stars

Neutron stars are highly dense stars - which are almost wholly comprised of neutrons - originating from the aftermath of supernova of Type Ib, Ic or Type II of a massive progenitor star. Of particular interest for the determination of neutron star properties is the thermodynamics for the coexistence of nuclear clusters entering the equation of state of nuclear matter. We present some analytical developments obtained so far.

To cite this abstract, use the following reference: http://meetings.aps.org/link/BAPS.2014.TSS.S4.3

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Bulletin of the American Physical Society

Joint Spring 2014 Meeting of the Texas Sections of the APS, AAPT, and Zone 13 of the SPS

Volume 59, Number 2

Thursday–Saturday, March 20–22, 2014; Abilene, Texas

Session S4: Astrophysics II

Abstract: S4.00003 : Effects of clustering in the equation of state for neutron stars

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