Authors: Sarah Millholland, Gregory Laughlin
First Author’s Institution: Department of Astronomy, Yale University
Status: Accepted by The Astrophysical Journal, open access
It’s not an easy life being a hot Jupiter. Besides their eternal loss of privacy from being on the hitlist of astronomers since the very moment they are detected, theirs is a tale of intense drama. The extreme radiation and tidal flexing they experience due to their proximity to their host stars make them ideal targets for studying planetary science in extreme physical conditions, particularly since there are no hot Jupiter analogues in our solar system. One of these weirdos, and also one of the most studied hot Jupiters in the last few years, is WASP-12b. In addition to being one of the hottest hot Jupiters around (with equilibrium temperature ~ 2500 K) and losing mass at an exceptionally high rate, it is also the only known hot Jupiter inspiralling rapidly towards its star. It has been speculated that sustained tidal interactions between the star and the planet could be responsible for the observed orbital decay of the planet. The authors of today’s paper investigate the case of WASP-12b in this context to understand what might be driving its orbital decay.
Turning with the tide
Tidal interactions between a star and its planet act together to dissipate the orbital energy of the system in the interiors of the planet and the star. Think of the planet and the star acting like resistors that dissipate the gravitational energy of their orbits into heat due to tidal flexing in their interiors. This tidal dissipation is most effective in cases of high planetary orbital eccentricity and obliquity (angle between the orbital plane and spin axes of the planet). However, for a lonely hot Jupiter with no other planetary companion in the system, tidal torques from the host star over time would also force the planet to reach an equilibrium state with low orbital eccentricity and obliquity, resulting in tidal dissipation to diminish with time. The fact that WASP-12b’s orbit is decaying rapidly indicates that there is significant tidal dissipation at work in the system possibly driven by some other mechanism.The authors of today’s paper propose that the presence of another planet in the system (see Figure 1) could sustain the obliquity and hence a very effective tidal dissipation of WASP-12b.
Figure 1: Schematic of the spin-orbit interactions between WASP-12b and another planet in the system. In the case of spin-orbit resonance (called a Cassini state), the spin angular momentum vector S1 and orbital angular momentum vector L1 precess about a common axis at the same rate. (Figure 1 in the paper)
If there is another planet in the system, it’s likely that WASP-12b could have gotten locked in a state of spin-orbit resonance (known as a Cassini state, also observed in the case of Earth-moon system) which means that the rate of precession of its orbital axis is the same as the spin axis precession rate. This implies that a change in the orbital precession rate of WASP-12b due to dynamical interactions with the perturbing planet in the system will cause a change in its spin precession rate as well, resulting in a higher obliquity of WASP-12b.
The authors simulate the evolution of the WASP-12 system using an obliquity tide model which couples the relations governing the secular dynamical interactions between WASP-12b and another planet, and the tidal interaction between the star and WASP-12b. These interactions then combine to cause the inspiral. With very little fine-tuning of the properties of the perturbing planet and the efficiency of tidal dissipation (which is dependent on the unknown interior structure of WASP-12b), they are able to reproduce the observed inspiral rate consistent with the current observations of the system (Figure 2). An interesting result of their analyses using the obliquity tide model is that even if WASP-12b starts with a very low obliquity (< 1 degree), it can easily get locked into a Cassini state and attain high-obliquity within the lifetime of the planetary system.
Figure 2: Simulated evolution of WASP-12b’s obliquity (gray) and semi-major axis (purple) with respect to time from the obliquity tide model. Note that tidal dissipation due to obliquity tides is a runaway process: orbital decay (represented by the decreasing semi-major axis ) due to tidal dissipation leads to increasing obliquity because of the other planet forcing WASP-12b to maintain the spin-orbit resonance, and this further increases the efficiency of tidal dissipation.
So obliquity tides can cause the observed orbital decay – but how do we confirm that? The good news is that, based on the predictions of their obliquity tide model, the authors conclude that the perturber planet is very likely within the limits of detection of extreme precision radial velocity instruments coming up in the near future. Tighter constraints on transit duration variations or transit timing variations (a signature of orbital precession) from more precise long term photometric monitoring of the system by TESS could also help in strengthening the obliquity tide hypothesis. If confirmed, obliquity tides might additionally be able to explain WASP-12b’s extreme radius inflation and unusual features in its thermal phase curves and will provide compelling evidence for in situ formation of hot Jupiters. Since tidal interactions are intimately tied to the interiors of the planets, they could also be an unprecedented tool for X-raying the interior structure, formation histories, and demographics of exoplanets.