Extrasolar planets: XVI Canary Islands Winter School of Astrophysics

Cover......Page 1
Half-title......Page 3
Series-title......Page 5
Title......Page 7
Copyright......Page 8
Contents......Page 9
Contributors......Page 10
Participants......Page 11
Preface......Page 13
Acknowledgements......Page 16
1.2 Pulsar timing......Page 17
1.3 Periodic radial velocity variations......Page 19
1.4 Gravitational microlensing......Page 20
1.5 Astrometry......Page 22
1.6 Imaging......Page 23
1.7 Radio flux......Page 25
1.8.1 Single-star transits......Page 26
1.8.2 Eclipsing binary transits......Page 28
1.9. Phase-reflection variations......Page 29
1.10 Eclipsing binary minima timing......Page 30
1.11 Secondary effects in extrasolar planet detection methods......Page 33
1.12 Ranges and combinations of detection methods......Page 34
1.13. Future mission near-term targets: M-dwarf star systems......Page 36
REFERENCES......Page 38
2.1 Motivation and context......Page 40
2.2.1. Measuring high-precision radial velocities......Page 41
2.2.2. Wavelength calibration and long-term stability......Page 43
2.2.3. Intrinsic stellar limitations on radial-velocity searches......Page 47
2.3. Orbital properties of extrasolar planets......Page 52
2.3.1 Giant extrasolar planets in numbers......Page 53
2.3.3 Period distribution of giant extrasolar planets......Page 54
2.3.4 Period–mass distribution......Page 57
2.3.5 Giant planets in multiple stellar systems......Page 58
2.3.6 Giant planet eccentricities......Page 61
2.4 Below the mass of Neptune......Page 62
2.4.1 Gaseous- vs. solid-planet properties at short periods......Page 63
2.5. Multi-planet systems......Page 65
2.5.1 Mean motion resonance systems......Page 66
2.5.2 Dynamics: planet–planet interaction and stability......Page 68
2.6.1 Metallicity of stars hosting giant planets......Page 70
2.6.2 Metallicity of stars hosting Neptune-mass planets......Page 72
2.6.3 Primary-mass effect......Page 73
2.7. Follow-up of transiting planets......Page 74
2.8 Future of radial velocities......Page 76
REFERENCES......Page 77
3.2 Basic ideas concerning transiting planets......Page 81
3.2.1 Astrometric, radial velocity and transit signals......Page 82
3.2.3 Signal characteristics......Page 83
3.2.4. Transit search system choices and requirements......Page 85
3.2.5. Strategic choices in transit-detection systems......Page 86
3.3.1. Noise sources......Page 87
3.3.3 Observing time and duty cycle......Page 88
3.3.4 Measuring gross characteristics of transiting planets......Page 90
3.4 False alarms......Page 91
3.4.1 Eclipse shape and out-of-transit variations......Page 92
3.4.3 Multi-colour and high spatial resolution photometry......Page 93
3.4.5 High-precision radial velocity......Page 94
3.5.1 Fundamentals......Page 95
3.5.2 Expected spectra......Page 96
3.5.3 Observations of transit spectra......Page 97
3.5.4 Observations of secondary transits......Page 99
3.6 The future of technical civilization......Page 100
REFERENCES......Page 103
4.1.1 Observations: 12 years, 21 stars – no planets (yet)......Page 105
4.2.1 The ‘original’ Solar System perspective......Page 106
4.3 Introduction – trying to solve a big problem......Page 107
4.4 The plan......Page 108
4.5.1 Clouds......Page 109
4.5.2 Clouds and stars......Page 110
4.5.3 How to begin – stellar evolution as initial value problem......Page 114
4.5.4 Early stellar evolution theory......Page 115
4.5.5 Strategies to determine ‘initial’ stellar structure......Page 116
4.6 Calculating protostellar collapse......Page 118
4.6.1 Inertia governs the collapse......Page 119
4.6.3 The heat in young stars......Page 120
4.6.4 Beyond the equilibria of stellar evolution theory......Page 121
4.7 Early stellar evolution – hydrostatic versus collapse......Page 122
4.8 Protoplanetary discs......Page 125
4.9 The Solar System......Page 127
4.10 Solar System formation......Page 128
4.11 Planet formation – the problem......Page 129
4.12 How to compress by 1010?......Page 130
4.14 From dust to planets......Page 131
4.15 Solar System formation modelling......Page 133
4.15.1 Gaseous envelopes – giant planets......Page 134
4.15.2 Hydrodynamic accretion beyond the critical mass......Page 136
4.16 The importance of convection......Page 137
4.18 Dynamic diversity......Page 139
4.19.1 Planetesimal formation......Page 140
4.19.3 Late accretion and final eccentricities......Page 141
4.20 Theory – planet mania......Page 142
4.21 What is a planet?......Page 143
4.22 Why not abandon Solar System formation theory?......Page 144
4.23.1 What is planetary migration?......Page 145
4.23.2 Violent migration......Page 146
4.23.3 A closer look......Page 147
4.23.4 Is a planet a hole or not a hole?......Page 149
4.25.1 A Pegasi planet: formation and properties......Page 150
4.25.2 Mass accretion history – the first 100 million years......Page 151
4.25.3 Luminosity of a young Pegasi planet......Page 152
4.26.1 Is there no bias . . .?......Page 154
4.26.3 Brave-hearted searches – Icarus!......Page 155
4.27 Has the Solar System been misleading us?......Page 156
4.28 Observational tests of formation theory......Page 157
4.28.1 Migration test I: hot neptunes......Page 158
4.28.3 Migration test III: Hill sphere expansion......Page 159
4.31 Conclusion......Page 161
REFERENCES......Page 162
5.1 Introduction......Page 166
5.2.1 Lithium......Page 168
5.2.2. The 6Li-test......Page 170
5.3.2 Refractories......Page 172
5.4.2 Astrobiology......Page 175
REFERENCES......Page 176
6.1 Introduction......Page 178
6.2.1 Spectroscopic signatures of substellarity......Page 179
6.2.2 Unveiling the substellar realm......Page 180
6.3 Brown dwarfs: photometric and spectroscopic properties......Page 181
6.4.1 Brown dwarf companions to stars......Page 183
6.4.2 Binary brown dwarfs......Page 184
6.4.3 Planets around brown dwarfs......Page 185
6.5 Searches in stellar clusters and young stellar associations: the brown dwarf mass function......Page 186
6.5.1 Isolated planetary-mass objects......Page 187
6.5.2 Substellar discs......Page 188
6.6 Formation mechanisms......Page 189
REFERENCES......Page 190
7.1 Introduction......Page 194
7.2 Global structure of Solar System......Page 195
7.2.1 Mechanics: orbits......Page 197
7.2.2 Mechanics of extended bodies......Page 198
7.3.1 Planets and satellites......Page 200
7.3.2 Asteroids, Kuiper belt objects and comet populations......Page 208
7.3.3 Meteorites and planetary rings......Page 211
7.4.1 Origin and chemical composition......Page 212
7.4.2 Energy sources......Page 214
7.4.3 Vertical thermal structure......Page 215
7.4.4 Dynamics: general circulation......Page 218
7.4.5 Meteorology......Page 225
7.5.1 Planetary magnetic fields......Page 226
7.5.2 Interaction with the solar wind......Page 228
REFERENCES......Page 230
8.1 Introduction......Page 233
8.1.1 Long-term climate evolution on Earth......Page 234
8.2 Venus, Mars and the habitable zones around the Sun and other stars......Page 241
8.2.1 Venus: runaway and ‘moist’ greenhouses and loss of water......Page 242
8.2.2 The climate of early Mars......Page 243
8.2.3 Habitable zones around main sequence stars......Page 246
8.3 Abiotic oxygen levels on the Earth and Earthlike planets......Page 247
8.3.2 Escape of hydrogen to space / the difusion-limited flux......Page 248
8.3.3 Balancing the atmospheric hydrogen budget: first-order calculation......Page 250
8.3.4 More rigorous calculation of the atmospheric hydrogen budget......Page 252
8.3.5 Abiotic O2 levels......Page 254
8.4.1 A few thoughts on the rise of atmospheric O2......Page 255
8.4.2 The rise of ozone......Page 256
REFERENCES......Page 258
9.1 Introduction: the search for habitable worlds......Page 261
9.2 The search for spectroscopic biosignatures......Page 262
9.3.1 O3 as a tracer of O2-rich atmospheres......Page 264
9.4.1 Abiotic production of O2 and O3......Page 268
9.5 Reliability of biomarkers inside and outside the habitable zone......Page 271
9.5.2 Inside the habitable zone of K-, G- and F-stars......Page 273
9.5.3 Beyond the outer edge of the habitable zone......Page 274
9.6 Other biosignatures?......Page 275
9.7 Temperature and radius of the planets......Page 278
9.8 The benefits from both infrared and visible observations......Page 280
9.9 Conclusion and other perspectives......Page 281
REFERENCES......Page 282