Equation of state for compact stars Lecture 1 - LUTh

More documents

Recommendations

Info

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

Structure of envelope and crust Schematic structure of an envelope of a neutron star with the internal temperature ∼ 10 8 K. Pawe̷l Haensel (CAMK) EOS for compact stars Lecture 1, IHP Paris, France 6 / 54
Plasma parameters Outer envelope: one kind of nuclei (fully ionized atoms) (A, Z), A = N + Z. This is an approximation - one component plasma (OCP). Mean number density of nuclei (=ions) n N . (If several j-species of nuclei are present then mean number density of nuclei n N = j nj.) Electron mean number density ne = Zn N . Outer envelope, outer crust: all nucleons bound in nuclei =⇒ mean nucleon (=baryon) number density nb = A n N Inner envelope, inner crust nb = A ′ n N where A ′ ≡ A + A ′′ . Here A ′′ is the number of free (unbound) nucleons per one atomic nucleus. We have A ′′ n N = nn (1 − w), where w is the fraction of volume occupied by atomic nuclei. Outer envelope A ′ = A, inner envelope A ′ > A. Mass density ρ = E/c 2 , but in the envelope and crust ρ ≈ munb, where mu = 1.6605 × 10 −24 g is the atomic mass unit. Pawe̷l Haensel (CAMK) EOS for compact stars Lecture 1, IHP Paris, France 7 / 54
Page 1 and 2: Equation of state for compact stars
Page 3 and 4: Anticipation and prediction of neut
Page 5: EOS - an overview EOS of neutron st
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?