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

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181614FRTF II Critical TFRTF II fitting functionFRTF I Critical TFRTF I fitting function12T c (MeV)10864200.50.40.3x i0.20.10Figure3.4: Thecritical temperatureasagivenprotonfraction:Numerical resultandanalyticfitting function.Table 3.2: Surface tension analytic fitting function for finite range modelModel ω 0 (x i = 0.5) α qTruncated 1.25728 3.6 39.0552New 1.02824 3.7 56.047950
1.41.2FRTF II ω 0 , T=0 MeVFRTF II fitting functionFRTF I ω 0 , T=0 MeVFRTF I fitting function1ω 0 (MeV/fm 2 )0.80.60.40.200.50.40.3x i0.20.10Figure 3.5: Surface tension at T = 0 MeV as a given proton fraction: Numerical result andanalytic fitting function.51
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Theory of nuclear matter of neutron
Page 3 and 4:
Abstract of the DissertationTheory
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To Jaenyeong, Jonghyun, and Jongbum
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3.3 Optimized Parameter Set . . . .
Page 9 and 10:
List of Figures1.1 Mass and radius
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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
Page 57 and 58: We choose the value ǫ = 1/3. One m
Page 59 and 60: where∆V t = T oρ o[( ρρ o) ǫ[
Page 61 and 62: Q 1 to a small number also results
Page 63 and 64: where p = (S v ,L) and M ij = 1 ∂
Page 65: 3.4 Nuclear Surface TensionCompared
Page 69 and 70: For the finite-range term, we use a
Page 71 and 72: Landau’s quasi-particle formula g
Page 73 and 74: The symmetry energy in nuclear matt
Page 75 and 76: Figure 4.2: The left figure shows t
Page 77 and 78: Figure 4.4: This figure shows the b
Page 79 and 80: Figure 4.5: In a neutron star, heav
Page 81 and 82: The energy exchange from the gradie
Page 83 and 84: Figure 4.8: The left panel shows th
Page 85 and 86: 4.5 Astrophysical application4.5.1
Page 87 and 88: 0.550.5GaussianFRTF IIFRTF I0.450.4
Page 89 and 90: neutron matter respectively. Those
Page 91 and 92: Table 5.3: Nuclear properties of si
Page 93 and 94: which aref Rc = a 0 +a 1 x+a 2 x 2
Page 95 and 96: parametrized[ht]504540EDF, Z nucFit
Page 97 and 98: Chapter 6Nuclear Equation of State
Page 99 and 100: Coulomb, and, symmetry part [24], i
Page 101 and 102: We can eliminate N s , leading to t
Page 103 and 104: pressure from pure neutron matter,
Page 105 and 106: 2.52GSRsSGISIVSkaSkI1SkI2SkI3SkI5St
Page 107 and 108: HNsn, p, α,eFigure 6.7: In the Wig
Page 109 and 110: Table 6.1: Surface tension analytic
Page 111 and 112: free energy density for the alpha p
Page 113 and 114: Here s ′ = ∂s(u)/∂u.The minim
Page 115 and 116: 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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