Theory of Nuclear Matter for Neutron Stars and ... - Graduate Physics

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energy and the density derivative of symmetry energy. We summarize recent experimentalresults, astrophysical inference, and theoretical pure neutron mattercalculations. The correlation between symmetry energy and the surface symmetryenergy in liquid droplet model is also obtained. The beta equilibrium matteris used to model the neutron star crust.The second part of the thesis is devoted to construction of a code to computethe nuclear EOS for hot dense matter that would be distributed to astrophysicscommunity. With this code, users will be able to generate tables with adjustableparameters describing the symmetry, incompressibility, and thermal propertiesof nuclear matter. We use the liquid droplet approach to generate thermodynamicallyconsistent nuclear EOS. table. Compared to previous attempts, weinclude neutron skin, Coulumb diffusion, and Coulomb exchange. In addition,we compute the surface tension as a function of proton fraction and temperatureconsistently with the bulk energy. For comparison, we generate an EOS tableusing the SLy4 non-relativistic Skyrme force model. For both FRTF and SLy4,more than 10 % of entries of EOS tables consists of nuclei, alpha particles, andnucleons.iv
To Jaenyeong, Jonghyun, and Jongbum
Page 1 and 2: Theory of nuclear matter of neutron
Page 3: Abstract of the DissertationTheory
Page 7 and 8: 3.3 Optimized Parameter Set . . . .
Page 9 and 10: List of Figures1.1 Mass and radius
Page 11 and 12: SymbolsNuclear Physics SymbolE ener
Page 13 and 14: ω δt 90−10QtT cTaylor expansion
Page 15 and 16: List of Tables1.1 Range of Tables .
Page 17 and 18: Chapter 1IntroductionStars give us
Page 19 and 20: Since the mass of neutron star is d
Page 21 and 22: shown in Fig. 1.2, LS220 is the onl
Page 23 and 24: density:p = ρ2ρ o[ K9µ n = −B
Page 25 and 26: nuclear energy density functional i
Page 27 and 28: 2.3.2 Thermodynamic QuantitiesThe t
Page 29 and 30: point r and with momentum p isU n (
Page 31 and 32: Thus, in the case of zero temperatu
Page 33 and 34: For standard nuclear matter, u = 1
Page 35 and 36: a α L α U β L β U σ0.5882 1.11
Page 37 and 38: Figure 2.2: Bulk equilibrium of T =
Page 39 and 40: Figure 2.4: Coexistence curves for
Page 41 and 42: proton fraction x are irrelevant fo
Page 43 and 44: potential model analogue for the Ha
Page 45 and 46: with the convention that z II is th
Page 47 and 48: Figure 2.10: The surface tension of
Page 49 and 50: Figure 2.12: Contour plots of surfa
Page 51 and 52: 2.6.2 Dense Matter and the Wigner-S
Page 53 and 54: Figure 2.15: Proton number per unit
Page 55 and 56:
Chapter 3Modified model† The trun
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We choose the value ǫ = 1/3. One m
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where∆V t = T oρ o[( ρρ o) ǫ[
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Q 1 to a small number also results
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where p = (S v ,L) and M ij = 1 ∂
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3.4 Nuclear Surface TensionCompared
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1.41.2FRTF II ω 0 , T=0 MeVFRTF II
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For the finite-range term, we use a
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Landau’s quasi-particle formula g
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The symmetry energy in nuclear matt
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Figure 4.2: The left figure shows t
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Figure 4.4: This figure shows the b
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Figure 4.5: In a neutron star, heav
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The energy exchange from the gradie
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Figure 4.8: The left panel shows th
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4.5 Astrophysical application4.5.1
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0.550.5GaussianFRTF IIFRTF I0.450.4
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neutron matter respectively. Those
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Table 5.3: Nuclear properties of si
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which aref Rc = a 0 +a 1 x+a 2 x 2
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parametrized[ht]504540EDF, Z nucFit
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Chapter 6Nuclear Equation of State
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Coulomb, and, symmetry part [24], i
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We can eliminate N s , leading to t
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pressure from pure neutron matter,
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2.52GSRsSGISIVSkaSkI1SkI2SkI3SkI5St
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HNsn, p, α,eFigure 6.7: In the Wig
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Table 6.1: Surface tension analytic
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free energy density for the alpha p
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Here s ′ = ∂s(u)/∂u.The minim
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6.5.2 Determination of Coulomb surf
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gives analytic derivatives of therm
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200180160Atomic number, Y p =0.45,
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for Fermi integral. This fitting fu
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A.1 Taylor expansion integrationThe
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thenwhere0u − i+1 = fu− i +J
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We separate the two integrals as in
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Each w i can be obtained[ae −∆/
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By expanding e r 0/a −e −r 0/a
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M 3 2a 0.433 1p 0 (e 2 /a) √ π/3
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of find exact polynomial expression
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Appendix CPhase coexistenceBulk equ
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To summarize, we need to solve 5 eq
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D.1 Non-uniform electron density ap
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Appendix ENuclear Quantities in Non
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Table E.1: Non-relativistic Skyrme
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[20] C.J. Pethick and D.G. Ravenhal
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Theory of Nuclear Matter for Neutron Stars and ... - Graduate Physics

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