Stability of planets in triple star systems
A thesis submitted to the Faculty of Science, University of the Witwatersrand South Africa in fulfilment of the requirements for the degree of Doctor of Philosophy. April 2018. === This study investigates the space around triple systems to find the regions of secular stability of planetary orbits...
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| Format: | Others |
| Language: | en |
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2018
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| Online Access: | Busetti, Franco Raoul (2018) Stability of planets in triple star systems, University of the Witwatersrand, Johannesburg, <http://hdl.handle.net/10539/26052> https://hdl.handle.net/10539/26052 |
| Summary: | A thesis submitted to the
Faculty of Science, University of the Witwatersrand South Africa
in fulfilment of the requirements for the degree of
Doctor of Philosophy. April 2018. === This study investigates the space around triple systems to find the regions of secular stability of planetary orbits. Numerical N-body simulations are used to determine empirically the bounds of these regions as a function of the system’s configuration.
There have been numerous theoretical studies of the stellar dynamics of triple systems, some with limited numerical checks, but the few purely empirical studies have been confined largely to binaries. Very little has been done on planetary orbits within either of these systems. There has been almost no work on generalised systems, little on retrograde planetary orbits and none on retrograde stellar orbits, with nearly all being on coplanar orbits and for a limited number of orbital parameters.
This work expands into, and investigates new areas through
1. Providing a generalised mapping of the regions of planetary stability in triples, by:
2. examining all four types of orbits – P1, P2, S1 and S3;
3. investigating these orbit types for both prograde and retrograde motion of the planets;
4. investigating them for both prograde and retrograde motion of the outer body of the triple;
5. investigating highly-inclined orbits of the outer star, stellar Kozai resonance and its effect on the region of stability for P1 and P2 orbits;
6. extending the number of parameters used to all relevant orbital elements of the triple’s stars, and
7. expanding these elements and mass ratios to wider ranges that will accommodate recent and possible future observational discoveries.
This resulted in semi-analytical models describing the stability bounds of each type of orbital configuration found in triples.
These relationships can be used to guide searches for planets in triple systems and to determine quickly the feasibility of initial observational estimates of planetary orbital parameters, and to select suitable candidates for a survey of such systems. The geometry of the stable zone indicates not only where to look for planets but the most suitable search method.
To highlight how the stability of planets in triple systems differs from that for binaries, an analysis of these systems over the same parameter space was required, resulting in a contribution to the body of empirical work on binaries as well.
Key words: methods: numerical – methods: N-body simulations – planet-star interactions – celestial mechanics – stars: hierarchical triples – planetary systems: dynamical evolution and stability === LG2018 |
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