Haghighipour Planets in Binary Star Systems

1. Auflage 2010
ISBN: 978-90-481-8687-7
Verlag: Springer Netherlands
Format: PDF
Kopierschutz: 1 - PDF Watermark

E-Book, Englisch, Band 366, 332 Seiten

Reihe: Astrophysics and Space Science Library

In 1988, in an article on the analysis of the measurements of the variations in the radial velocities of a number of stars, Campbell, Walker, and Yang reported an - teresting phenomenon;the radial velocity variations of Cephei seemed to suggest the existence of a Jupiter-like planet around this star. This was a very exciting and, at the same time, very surprising discovery. It was exciting because if true, it would have marked the detection of the ?rst planet outside of our solar system. It was surprising because the planet-hosting star is the primary of a binary system with a separation less than 19 AU, a distance comparable to the planetary distances in our solar system. The moderatelyclose orbit of the stellar companionof Cephei raised questions about the reality of its planet. The skepticism over the interpretation of the results (which was primarily based on the idea that binary star systems with small sepa- tions would not be favorable places for planet formation) became so strong that in a subsequent paper in 1992, Walker and his colleagues suggested that the planet in the Cephei binary might not be real, and the variations in the radial velocity of this star might have been due to its chromospheric activities.

Autoren/Hrsg.

Haghighipour, Nader

Inhaltsverzeichnis

1;Preface
;5
2;Contents;7
3;1 Disks Around Young Binary Stars;9
3.1;1.1 Introduction;9
3.2;1.2 Inner Disks;13
3.3;1.3 Outer Disks;16
3.4;1.4 Orientation of Disks in Young Binaries;18
3.5;1.5 Debris Disks and Binaries;20
3.6;1.6 Future Tests and Observations;22
3.7;References;25
4;2 Probing the Impact of Stellar Duplicity on Planet Occurrence with Spectroscopic and Imaging Observations;27
4.1;2.1 Introduction;27
4.2;2.2 Results from Classical Doppler Planet Searches;30
4.2.1;2.2.1 Selection Effects Against Binaries in Doppler Planet Searches;31
4.2.2;2.2.2 The Sample of Planets in Binaries;32
4.2.3;2.2.3 Different Properties for Planets in Binaries?;33
4.3;2.3 Results from Imaging Surveys;35
4.3.1;2.3.1 Our VLT/NACO Search for Stellar Companions to 130 Nearby Stars with and Without Planets;35
4.3.1.1;2.3.1.1 Sample and Observing Strategy;35
4.3.1.2;2.3.1.2 Observational Results;37
4.3.2;2.3.2 The Impact of Stellar Duplicity on Planet Occurrence;39
4.3.2.1;2.3.2.1 Preliminary Statistical Analysis Based on the NACO Survey;39
4.3.2.2;2.3.2.2 Concluding Remarks on the Results from Imaging Surveys;41
4.4;2.4 Results from Doppler Planet Searches in Spectroscopic Binaries;41
4.4.1;2.4.1 Planet Searches in Single-Lined Spectroscopic Binaries;42
4.4.1.1;2.4.1.1 Sample and Observations;43
4.4.1.2;2.4.1.2 First Analysis Based on One-Dimensional Cross-Correlation;43
4.4.1.3;2.4.1.3 Identifying the Origin of Residual-Velocity Variations;46
4.4.1.4;2.4.1.4 Preliminary General Results on Planet Searches in SB1s;46
4.4.2;2.4.2 Planet Searches in Double-Lined Spectroscopic Binaries;49
4.4.2.1;2.4.2.1 The Example of HD188753;49
4.4.2.2;2.4.2.2 Concluding Remarks on Planet Searches in SB2s;51
4.5;2.5 Conclusion and Perspectives;51
4.6;References;53
5;3 The Detection of Extrasolar Planets Using Precise Stellar Radial Velocities;58
5.1;3.1 Introduction;58
5.2;3.2 Traditional Methods of Stellar RV Measurements ;59
5.3;3.3 The Telluric Technique;62
5.4;3.4 Absorption Cells;63
5.4.1;3.4.1 The Hydrogen-Fluoride Absorption Cell;64
5.4.2;3.4.2 Iodine Absorption Cells;65
5.4.2.1;3.4.2.1 Details on the Use of the Iodine Absorption Cell;67
5.5;3.5 Simultaneous Thorium-Argon Calibration;69
5.5.1;3.5.1 Iodine Cells Versus Simultaneous Th-Ar;72
5.5.1.1;3.5.1.1 Advantages of Th-Ar;72
5.5.1.2;3.5.1.2 Disadvantages of Th-Ar;73
5.5.2;3.5.2 Spectrograph Requirements for Precise RV Measurements;75
5.6;3.6 Extrasolar Planets in Binary Systems;76
5.6.1;3.6.1 16 Cyg B;77
5.6.2;3.6.2 Cep;79
5.7;References;82
6;4 Observational Techniques for Detecting Planets in Binary Systems;84
6.1;4.1 Why Focus Planet Searches on Binary Stars?;84
6.2;4.2 S-Type Planets;85
6.2.1;4.2.1 Wide Binaries;85
6.2.1.1;4.2.1.1 Dual-Star Astrometry;86
6.2.1.2;4.2.1.2 Radial Velocities;90
6.2.1.3;4.2.1.3 Observational Precisions;91
6.2.2;4.2.2 Close Binaries;92
6.2.2.1;4.2.2.1 PHASES Astrometry;93
6.2.2.2;4.2.2.2 Radial Velocities;95
6.2.2.3;4.2.2.3 Eclipse Timing;97
6.3;4.3 P-Type (Circumbinary) Planets;103
6.3.1;4.3.1 Radial Velocities;103
6.3.2;4.3.2 Eclipse Timing;105
6.4;References;107
7;5 The SARG Planet Search;111
7.1;5.1 Introduction;111
7.2;5.2 Properties of Planets in Binary Systems;112
7.3;5.3 Binary Systems as a Tool to Study the Ingestion of Planetary Material by the Central Star;118
7.4;5.4 The SARG Sample;119
7.5;5.5 Observations;120
7.6;5.6 Abundance Analysis;121
7.6.1;5.6.1 The Special Case of the Blue Straggler HD 113984;122
7.6.2;5.6.2 Abundance Difference Between Components of Binary Systems with Planetary Companions;124
7.7;5.7 Radial Velocities;125
7.7.1;5.7.1 Planet Candidates and Low Amplitude Variables;125
7.7.2;5.7.2 New Triple Systems and Stars with Long Term Trends;127
7.8;5.8 Line Bisectors: A Tool to Study Stellar Activity and Contamination;129
7.9;5.9 Upper Limits on Planetary Companions;132
7.10;5.10 On the Frequency of Planets in Binary Systems;132
7.11;References;138
8;6 Early Evolution of Planets in Binaries: Planet–Disk Interaction;140
8.1;6.1 Introduction;140
8.1.1;6.1.1 Summary of Observations;140
8.1.2;6.1.2 Summary of Planet Formation in Binaries;141
8.2;6.2 Evolution of Planets in Circumstellar Disks with a Companion;143
8.2.1;6.2.1 Disk Evolution in the Presence of a Companion;143
8.2.1.1;6.2.1.1 Numerical Setup;144
8.2.1.2;6.2.1.2 The Structure of the Disk;145
8.2.1.3;6.2.1.3 The Orbital Elements of the Binary;146
8.2.1.4;6.2.1.4 The Behaviour of an Embedded Planet;149
8.2.1.5;6.2.1.5 Comparison with Cep;153
8.3;6.3 Evolution of Planetesimals in a Circumstellar Disk with a Companion;154
8.4;6.4 Evolution of Planets in Circumbinary Disks;157
8.4.1;6.4.1 Low Mass Circumbinary Planets;157
8.4.2;6.4.2 High Mass Circumbinary Planets;161
8.4.2.1;6.4.2.1 Mode 1 – Planetary Scattering;162
8.4.2.2;6.4.2.2 Mode 2 – Near-Resonant Protoplanet;162
8.4.2.3;6.4.2.3 Mode 3 – Eccentric Disk;165
8.5;6.5 Conclusions;167
8.6;References;168
9;7 Dynamics and Planet Formation in/Around Binaries;170
9.1;7.1 Introduction;170
9.1.1;7.1.1 The ``Standard'' Planet Formation Scenario;170
9.1.2;7.1.2 Planets in Binary Star Systems;172
9.2;7.2 Planetesimal Dynamics in a Binary Star System: the Secular Approximation;174
9.3;7.3 Effects of the Secular Perturbations on "426830A v "526930B ;175
9.4;7.4 Role of Gas Drag;179
9.5;7.5 Dependence of the Accretion Process on the Binary Parameters;182
9.6;7.6 Inclined Binaries;186
9.7;7.7 Type II Runaway Growth;188
9.8;7.8 Conclusions;194
9.9;References;195
10;8 Gravitational Instability in Binary Protoplanetary Disks;199
10.1;8.1 Introduction;199
10.1.1;8.1.1 Gravitational Instabilities;200
10.1.2;8.1.2 Fragmentation and Survival of Clumps;201
10.2;8.2 Numerical Techniques and Assumptions;203
10.2.1;8.2.1 Hydrodynamics Methods;203
10.2.2;8.2.2 Gravity Solvers;205
10.2.3;8.2.3 Timestepping;208
10.2.4;8.2.4 Artificial Viscosity;209
10.2.5;8.2.5 Internal Energy Equation;211
10.2.6;8.2.6 Cooling in the Simulations;213
10.3;8.3 Initial and Boundary Conditions;217
10.3.1;8.3.1 Density and Temperature Profiles;218
10.3.2;8.3.2 Disk Masses and Toomre Parameters;220
10.3.3;8.3.3 Numerical Resolution;222
10.3.4;8.3.4 Boundary Conditions;222
10.3.5;8.3.5 Orbital Parameters;223
10.4;8.4 Gravitational Instability in Binary Systems;223
10.4.1;8.4.1 Does Binarity Help or Suppress Disk Fragmentation?;223
10.4.2;8.4.2 Disk Evolution: Internal vs. External;229
10.4.3;8.4.3 Temperatures in Binary Self-Gravitating Disks and Effects on Dust Grains;230
10.4.4;8.4.4 Effects of Artificial Viscosity;232
10.4.5;8.4.5 Initial Conditions in the Context of Star Formation;233
10.5;8.5 Conclusions;236
10.6;References;240
11;9 N-Body Integrators for Planets in Binary Star Systems;243
11.1;9.1 Introduction;243
11.2;9.2 Mixed-Variable Symplectic Integrators;244
11.3;9.3 Binary-Star Algorithms;247
11.3.1;9.3.1 Modifying the Wisdom–Holman Mapping;247
11.3.2;9.3.2 Wide Binary Case;250
11.3.3;9.3.3 Close Binary Case;254
11.4;9.4 Symplectic Correctors;256
11.5;9.5 Stellar Encounters;261
11.6;9.6 Conclusions;265
11.7;References;266
12;10 Terrestrial Planet Formation in Binary Star Systems;268
12.1;10.1 Introduction;268
12.2;10.2 Model and Initial Conditions;269
12.3;10.3 Planet Formation in the Centauri AB Binary Star System;270
12.4;10.4 S-type Orbits in Other `Wide' Binary Star Systems;274
12.5;10.5 P-type Orbits Within Close Binary Star Systems;277
12.6;10.6 Conclusions;282
12.7;References;285
13;11 Planetary Dynamics and Habitable Planet Formation in Binary Star Systems;287
13.1;11.1 Introduction;287
13.2;11.2 Planetary Motion in Binary Systems and Stability;289
13.2.1;11.2.1 Stability of S-Type Orbits;292
13.2.1.1;11.2.1.1 Application to the Binary Cephei;297
13.2.1.2;11.2.1.2 Application to Binaries Gliese 86 and HD41004;300
13.2.2;11.2.2 Stability of P-Type Orbits;301
13.2.3;11.2.3 Stability of L-Type Orbits;302
13.3;11.3 Terrestrial Planets in Binaries;303
13.3.1;11.3.1 Stability of TP-i and TP-o Orbits;304
13.3.2;11.3.2 Stability of TP-t Orbits;310
13.4;11.4 Habitable Planet Formation in Binaries;312
13.4.1;11.4.1 Habitable Zone;315
13.4.2;11.4.2 Formation of Habitable Planets in S-Type Binaries;317
13.5;References;326
14;Index;330