Eccentricities and Stellar Obliquities in Hot and Warm Jupiter Systems with External Perturbers

Add to your list(s) Download to your calendar using vCal

• Kassandra Anderson (Cornell University)
• Monday 15 October 2018, 14:00-15:00
• MR14, Centre for Mathematical Sciences, Wilberforce Road, Cambridge.

If you have a question about this talk, please contact Dr William Béthune.

Hot Jupiters (HJs) and warm Jupiters (WJs) exhibit several observational puzzles, including stellar spin-orbit misalignments (obliquities) in many HJ systems, and substantial eccentricities in many WJ systems. This talk considers the role of an external planetary companion in generating such eccentricities and stellar obliquities. In Part I of the talk, we investigate whether an external companion may induce secular eccentricity oscillations in WJ systems, through an apsidal precession resonance (when the companion is eccentric and co-planar), or Lidov-Kozai oscillations (when the companion is sufficiently inclined). We consider the sample of WJs with detected outer companions, and for each system, identify the range of mutual inclinations needed to generate the observed WJ eccentricity. For most systems, we find that high inclinations are needed so that Lidov-Kozai cycles are induced; the outer companions are typically not eccentric enough to generate the observed WJ eccentricity in a low-inclination configuration. Observational constraints on mutual inclinations in two-planet systems are needed to clarify the role of external companions in secularly exciting WJ eccentricities. In Part II of the talk, we consider the possibility of an inclined companion in exciting the stellar obliquity due to a secular resonance, occurring when the precession rate of the stellar spin axis (driven by the inner planet) becomes comparable to the nodal precession rate of the inner planet (driven by the outer planet). Due to their close proximity to the host star, HJs have strongly-coupled stellar spin and orbital axes, and a strong perturber is required to raise the obliquity, located within 1-2 AU. In contrast, WJ systems experience weaker spin-orbit coupling, and obliquity excitation may be achieved for more distant perturbers, located at tens of AU. Unlike HJs, WJ stellar obliquities have not been extensively probed. We predict WJs may have significant obliquities due to resonant excitation, especially those orbiting cool host stars.

This talk is part of the DAMTP Astrophysics Seminars series.

This talk is included in these lists:

• All CMS events
• CMS Events
• Cambridge Astronomy Talks
• Cosmology, Astrophysics and General Relativity
• DAMTP Astrophysics Seminars
• DAMTP info aggregator
• Interested Talks
• MR14, Centre for Mathematical Sciences, Wilberforce Road, Cambridge
• bld31

Note that ex-directory lists are not shown.