Equation of state for compact stars Lecture 1 - LUTh

More documents

Recommendations

Info

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

Neutron star interior: known and unknown Plan White dwarfs and neutron star envelopes Neutron star crusts Neutron star cores: nucleons and hyperons Briefly - exotic neutron star cores, quark stars, etc. Briefly - confronting EOS models with mesured neutron star masses Standard reference: S.L. Shapiro, S.A. Teukolsky Black Holes, White Dwarfs, and Neutron Stars: The Physics of Compact Objects (Wiley, 1983). Alas, 23-years old. New advanced reference available soon: P. Haensel, A.Y. Potekhin, and D.G. Yakovlev Neutron Stars 1. Equation of state and structure (Springer, January 2007) Pawe̷l Haensel (CAMK) EOS for compact stars Lecture 1, IHP Paris, France 4 / 54
EOS - an overview EOS of neutron star matter at T = 0: Baym et al. (1971) (triangles), Haensel & Pichon (1994)(HP94, stars), SLy - Douchin & Haensel (2001) (dots). Finite T EOSs: OPAL (Rogers et al. 1996) at T = 10 6 , 10 7 , and 10 8 K (dashed lines), the fit (Haensel & Potekhin 2004)(the solid line) and the fit modified at low ρ (the dotted line). From Haensel & Potekhin (2004). For ρ > 10 6 g cm −3 T -effects invisible - matter fully degenerate, T = 0 approximation for the EOS is valid. Pawe̷l Haensel (CAMK) EOS for compact stars Lecture 1, IHP Paris, France 5 / 54
Page 1 and 2: Equation of state for compact stars
Page 3: Anticipation and prediction of neut
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 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

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

Delete template?

Save as template?