Equation of state for compact stars Lecture 1 - LUTh
Equation of state for compact stars Lecture 1 - LUTh
Equation of state for compact stars Lecture 1 - LUTh
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Thomas-Fermi method - continued<br />
To determine the ground <strong>state</strong> at a given nb, one has to find nn(r) and np(r),<br />
which minimize Ecell/Vc under the constraints<br />
<br />
Vcnb = [nn(r) + np(r)] d 3 <br />
r , [np(r) − ne] d 3 r = 0 . (47)<br />
cell<br />
The problem is simplified assuming spherical symmetry; in this case the unit cell is<br />
approximated by a sphere <strong>of</strong> the radius rc = (3Vc/4π) 1/3 . The boundary<br />
conditions are such that far from the nucleus surface the nucleon densities are<br />
uni<strong>for</strong>m. This requires the nuclear radius to be significantly smaller than rc.<br />
Pawe̷l Haensel (CAMK) EOS <strong>for</strong> <strong>compact</strong> <strong>stars</strong> <strong>Lecture</strong> 1, IHP Paris, France 42 / 54<br />
cell
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