Ecole doctorale de Physique de la région Parisienne (ED107)

More documents

Recommendations

Info

204 Bibliographie Thorne, K. S., Campolattaro, A., Erratum : Non-Radial Pulsation of General- Relativistic Stellar Models. I. Analytic Analysis for l ≥ 2, ApJ , 152 : 673 (1968). Tilley, D. R., Tilley, J., Superfluidity and Superconductivity, John Wiley and Sons, Inc., New York (1974). Tourrenc, P., Relativité et Gravitation, Armand Colin, Paris, 267 pages (1992). Unno, W., Osaki, Y., Ando, H., Shibahashi, H., Nonradial oscillations of stars, Tokyo, University of Tokyo Press, First edition 1979, Tokyo, 420 pages (1989). Villain, L., Bonazzola, S., Inertial modes in slowly rotating stars : An evolutionary description, Physical Review D, 66 : 123001, 25 pages (2002). Villain, L., Haensel, P., Non-equilibrium beta processes in superfluid neutron star cores, en préparation (2003). Wald, R. M., General relativity, Chicago, University of Chicago Press, 504 pages (1984). Walter, F. M., Matthews, L. D., The optical counterpart of the isolated neutron star RX J185635-3754, Nature, 389 : 358–360 (1997). Walter, F. M., Wolk, S. J., Neuhauser, R., Discovery of a nearby isolated neutron star, Nature, 379 : 233–235 (1996). Wilson, J. R., Mathews, G. J., Relativistic hydrodynamics, Evans, C. R., Finn, L. S., Hobill, D. (eds.), Frontiers in numerical relativity, Cambridge Univ. Press, pages 306– (1989). Wiringa, R. B., Fiks, V., Fabrocini, A., Equation of state for dense nucleon matter, Physical Review C , 38 : 1010–1037 (1988). Witten, E., A New Proof of the Positive Energy Theorem, Commun. Math. Phys., 80 : 381–402 (1981). Wolf, R. A., Some Effects of the Strong Interactions on the Properties of Neutron-Star Matter, ApJ , 145 : 834–841 (1966). Yakovlev, D. G., Kaminker, A. D., Gnedin, O. Y., 1 S0 neutron pairing vs. observations of cooling neutron stars, A&A, 379 : L5–LL8 (2001a). Yakovlev, D. G., Kaminker, A. D., Gnedin, O. Y., Haensel, P., Neutrino emission from neutron stars, Phys. Rep., 354 : 1–155 (2001b). Yakovlev, D. G., Kaminker, A. D., Haensel, P., Gnedin, O. Y., The cooling neutron star in 3C 58, A&A, 389 : L24–LL27 (2002). Yakovlev, D. G., Levenfish, K. P., Modified URCA process in neutron star cores., A&A, 297 : 717–726 (1995). Yakovlev, D. G., Levenfish, K. P., Shibanov, Y. A., Cooling Neutron Stars and Superfluidity in Their Interiors, Phys. Usp., 42 : 737–821 (1999). Yoshida, S., Lee, U., Relativistic r-Modes in Slowly Rotating Neutron Stars : Numerical Analysis in the Cowling Approximation, ApJ , 567 : 1112–1120 (2002).
Page 1:
Ecole doctorale de Physique de la r
Page 5 and 6:
Table des matières Résumé v Abst
Page 7 and 8:
TABLE DES MATIÈRES iii 4.5.2 Noise
Page 9 and 10:
Résumé Résumé v Cette étude tr
Page 11 and 12:
Abstract Abstract vii This study de
Page 13 and 14:
Introduction Les sens dont l’a do
Page 15 and 16:
Introduction 3 même, leurs observa
Page 17 and 18:
Chapitre 1 Relativité générale e
Page 19 and 20:
1.1 Relativité générale 1.1.1 Gr
Page 21 and 22:
1.1 Relativité générale 9 La rel
Page 23 and 24:
1.1.3 Tests et prédictions 1.1 Rel
Page 25 and 26:
1.2 Ondes gravitationnelles 1.2.1 E
Page 27 and 28:
y 1.2 Ondes gravitationnelles 15 x
Page 29 and 30:
1.3 Sources d’ondes gravitationne
Page 31 and 32:
Page 33 and 34:
Page 35 and 36:
1.4 Détection 23 Figure 1.6 - Sens
Page 37 and 38:
¢¡ £ © ¥ ¢¡ £ © ¤ ¢¡ £
Page 39 and 40:
Chapitre 2 Etoiles à neutrons Somm
Page 41 and 42:
2.1 Naissance d’une étoile à ne
Page 43 and 44:
2.1 Naissance d’une étoile à ne
Page 45 and 46:
astre Terre Soleil naine blanche é
Page 47 and 48:
2.2 Structure interne 35 Figure 2.4
Page 49 and 50:
2.2 Structure interne 37 extensions
Page 51 and 52:
2.2 Structure interne 39 Figure 2.5
Page 53 and 54:
2.2 Structure interne 41 rigidité
Page 55 and 56:
2.2 Structure interne 43 où = h/2
Page 57 and 58:
2.2 Structure interne 45 à des fer
Page 59 and 60:
2.2 Structure interne 47 Type de su
Page 61 and 62:
2.3 Principes de l’évolution d
Page 63 and 64:
Page 65 and 66:
est environ 0.7 fois la masse nue 1
Page 67 and 68:
Page 69 and 70:
Page 71 and 72:
Log 10 (T/10 9 K) 0 -0.5 -1 -1.5 -2
Page 73 and 74:
2.4 Superfluidité et écarts à l
Page 75 and 76:
Page 77 and 78:
aboutit à 2.4 Superfluidité et é
Page 79 and 80:
Page 81 and 82:
Page 83 and 84:
Résultats 2.4 Superfluidité et é
Page 85 and 86:
Page 87 and 88:
Page 89 and 90:
Chapitre 3 Oscillations stellaires
Page 91 and 92:
3.1 Modes d’une étoile à neutro
Page 93 and 94:
3.1.2 Perturbations 3.1 Modes d’u
Page 95 and 96:
Un mode propre vérifie donc 3.1 Mo
Page 97 and 98:
3.1 Modes d’une étoile à neutro
Page 99 and 100:
3.2 Oscillations d’une étoile re
Page 101 and 102:
Page 103 and 104:
Page 105 and 106:
Page 107 and 108:
Ω c /Ω max 1.00 0.98 0.96 0.94
Page 109 and 110:
3.3 Modes inertiels et r-modes 97 F
Page 111 and 112:
P K /P 1.0 0.8 0.6 0.4 0.2 3.3 Mode
Page 113 and 114:
3.3 Modes inertiels et r-modes 101
Page 115 and 116:
Chapitre 4 Inertial modes in slowly
Page 117 and 118:
4.1 Introduction 105 what is done w
Page 119 and 120:
4.2 Equations and numbers 107 obvio
Page 121 and 122:
4.2 Equations and numbers 109 tenso
Page 123 and 124:
4.2 Equations and numbers 111 4.2.2
Page 125 and 126:
or 4.2 Equations and numbers 113 Tv
Page 127 and 128:
4.3 Mass conservation, boundary con
Page 129 and 130:
4.4 Test and calibration of the cod
Page 131 and 132:
4.4 Test and calibration of the cod
Page 133 and 134:
Sp(V θ ) 1 4.4 Test and calibratio
Page 135 and 136:
E(t) / E 0 1.15 1.1 1.05 1 4.4 Test
Page 137 and 138:
Sp(S xx ) S xx 0.1 0 -0.1 4.4 Test
Page 139 and 140:
V r Sp(V r ) 0.4 0.2 0 -0.2 -0.4 -0
Page 141 and 142:
4.5.1 Modifications 4.5 Differentia
Page 143 and 144:
Sp(V r ) V r 4 2 0 -2 4.5 Different
Page 145 and 146:
4.6 Strong Cowling approximation in
Page 147 and 148:
V θ Sp(V θ ) 10 5 0 -5 -10 4.6 St
Page 149 and 150:
can be written 4.6 Strong Cowling a
Page 151 and 152:
E Polar / E Total 0.05 0.04 0.03 0.
Page 153 and 154:
S xx Sp(S xx ) 0.2 0.1 0 -0.1 4.6 S
Page 155 and 156:
GW emission. 4.8 Acknowledgments 4.
Page 157 and 158:
Chapitre 5 Modes inertiels dans des
Page 159 and 160:
5.1 Etoiles relativistes en rotatio
Page 161 and 162:
Page 163 and 164:
Page 165 and 166: 5.1 Etoiles relativistes en rotatio
Page 167 and 168: 5.2 Equation d’état et hydrodyna
Page 171 and 172: où l’on a introduit 5.2 Equation
Page 175 and 176: 5.3 Résultats numériques 163 [voi
Page 177 and 178: 5.3 Résultats numériques 165 Il e
Page 179 and 180: 5.4 Conclusions 167 Spectres de pui
Page 181 and 182: Conclusions et perspectives “Pour
Page 183 and 184: Remerciements 171 La liste est long
Page 185 and 186: Appendice A Géométrie différenti
Page 187 and 188: A.3 Métrique et variétés (pseudo
Page 189 and 190: Appendice B Spectral methods and ve
Page 191 and 192: B.1 Spirit of the spectral methods
Page 193 and 194: B.1 Spirit of the spectral methods
Page 195 and 196: B.2 Solving Euler or Navier-Stokes
Page 197 and 198: The divergence-free approximation B
Page 199 and 200: Liste des tableaux Etoiles à neutr
Page 201 and 202: Table des figures Relativité gén
Page 203 and 204: TABLE DES FIGURES 191 4.14 Time evo
Page 205 and 206: Bibliographie Akmal, A., Pandharipa
Page 207 and 208: Bibliographie 195 Bonnor, W. B., Sp
Page 209 and 210: Bibliographie 197 Glendenning, N. K
Page 211 and 212: Bibliographie 199 Kokkotas, K. D.,
Page 213 and 214: Bibliographie 201 Murray, S. S., Sl
Page 215: Bibliographie 203 Ruoff, J., Stavri
show all

Ecole doctorale de Physique de la région Parisienne (ED107)

Create successful ePaper yourself

Delete template?

Save as template?