Equation of state for compact stars Lecture 1 - LUTh

More documents

Recommendations

Info

$J. Phys. A: Math. Gen. 32 (1999) - LUTH - Observatoire de Paris$

Hartree-Fock calculation of ground state crust Put A = N + Z nucleons and Z electrons in a box of volume Vcell (=unit cell) and calculate ground state of the system at fixed nb = A/Vcell. The A − body problem - solved using nuclear many-body theory. A ∼ 50 − 1000. ”Effective nuclear” Hamiltonian ˆH eff N = A ˆtj + j=1 k
Effective nucleon-nucleon interaction Most popular: Skyrme interaction. The basic assumption which justifies a Skyrme-type effective NN interaction (Skyrme 1956) is that its range is small as compared with the internucleon distances. This means, that in momentum representation the effective NN interaction ˆ v eff (k, k ′ ) can be approximated by a momentum independent term plus terms quadratic in the initial and final relative momenta of an interacting nucleon pair, k and k ′ , with the appropriate spin dependence. Numerical values of the parameters of effective interaction are to be determined from fitting masses of laboratory nuclei in ground states and low-lying excited states. The complete Hamiltonian of the unit cell is ˆ Heff cell = ˆ Heff N + VCoul + ˆ He, where VCoul describes Coulomb interaction between protons and electrons, and ˆHe corresponds to a uniform electron gas. Pawe̷l Haensel (CAMK) EOS for compact stars Lecture 1, IHP Paris, France 37 / 54
Page 1 and 2: Equation of state for compact stars
Page 3 and 4: Anticipation and prediction of neut
Page 5 and 6: EOS - an overview EOS of neutron st
Page 7 and 8: Plasma parameters Outer envelope: o
Page 9 and 10: Electrons - continued The density o
Page 11 and 12: ni = nN Ions The strength of the Co
Page 13 and 14: Ions - continued The scale-length t
Page 15 and 16: ρ − T diagram for the outer enve
Page 17 and 18: Pressure - electrons - main term (i
Page 19 and 20: Coulomb gas of ions (id)i Ideal cla
Page 21 and 22: N = N N = Ni = n N V Strongly coupl
Page 23 and 24: Melting - phase transition The soli
Page 25 and 26: Quantum zero-point vibrations and m
Page 27 and 28: Other corrections relevant to elect
Page 29 and 30: Ground state crust - T = 0 Notation
Page 31 and 32: Ground state crust - T = 0 The latt
Page 33 and 34: Ground state crust - T = 0 - nuclei
Page 35: Matter should be in equilibrium wit
Page 39 and 40: Nucleon density distribution in the
Page 41 and 42: Semi-classical - Thomas-Fermi metho
Page 43 and 44: Thomas-Fermi method - continued Neu
Page 45 and 46: Spherical unit cell radius rc, the
Page 47 and 48: Funny nuclei - ”nuclear pasta”
Page 49 and 50: Overall inner crust EOSs - SLy and
Page 51 and 52: Melting temperature Melting tempera
Page 53 and 54: Shear modulus of the crust Effectiv

Equation of state for compact stars Lecture 1 - LUTh

Create successful ePaper yourself

Delete template?

Save as template?