Equation of state for compact stars Lecture 1 - LUTh

More documents

Recommendations

Info

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

Z of nuclei in the inner crust Numbers of protons per nucleus in the ground state of the inner crust obtained by various authors. Solid lines: RBP – Ravenhall et al. (1972); FPS – as quoted by Pethick & Ravenhall (1995); DH – Douchin & Haensel (2000,2001). Crosses – Negele & Vautherin (1973). Pawe̷l Haensel (CAMK) EOS for compact stars Lecture 1, IHP Paris, France 46 / 54
Funny nuclei - ”nuclear pasta” Generally, while minimizing the energy, the nuclear shape has to be treated as a thermodynamic variable. The actual shape of nuclei in the ground state corresponds to the minimum of E at a given nb. Unit cells for a set of nuclear shapes (spheres, rods, plates) in the inner crust. The size of the unit cell is rc. Hatched regions show nuclear matter, while blank regions show neutron gas. In “bubbular phases” (tubes, spherical bubbles) one has to exchange the blank and hatched regions. Culinary names for ”pasta phases”: cylinders - spaghetti; plates - lasagna; spherical bubbles - Swiss cheese, . . . Pawe̷l Haensel (CAMK) EOS for compact stars Lecture 1, IHP Paris, France 47 / 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 and 36: Matter should be in equilibrium wit
Page 37 and 38: Effective nucleon-nucleon interacti
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: Spherical unit cell radius rc, the
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

You also want an ePaper? Increase the reach of your titles

Delete template?

Save as template?