Statistics
Scientific paper
Jan 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21536708f&link_type=abstract
American Astronomical Society, AAS Meeting #215, #367.08; Bulletin of the American Astronomical Society, Vol. 42, p.557
Statistics
Scientific paper
The angle between the stellar spin axis and the planetary orbit axis can be probed by the spectroscopic Rossiter-McLaughlin effect during planetary transits. Five systems have indicated misalignment; ten systems are consistent with alignment. The statistical analysis of Fabrycky & Winn (2009, ApJ, 696, 1230) is updated in the Table. A simple bimodal distribution of spin-orbit angles is favored over a simple unimodal distribution by a factor of 3 × 106. One possible interpretation is that (1) the majority of stellar spins and newborn planetary orbits are coplanar with their protoplanetary disks, so migration through that disk leads to spin-orbit alignment, and (2) a minority of hot Jupiters, though forming coplanar with the stellar equator, are later scattered or secularly torqued into misaligned, roughly isotropic, orbits.
In migration theories of the latter, a third body absorbs angular momentum and tidal dissipation removes energy. As the semi-major axis shrinks, the dominant precessional effect transfers from the third body to the stellar oblateness. The resulting secular resonance can excite a large spin-orbit misalignment, including slightly-retrograde polar orbits. In the case of Kozai cycles with tidal friction, the spin-orbit evolution of the archetypical case of HD 80606b can be framed as an adiabatic capture problem. The expected orbit-orbit inclination of 50° or 130° (which is unobservable) maps to final stellar obliquities of either 50° or 110°. Typically the prediction is less precise because tidal evolution is often faster than precession, yet two preferential obliquities still appear in population calculations (Fabrycky & Tremaine 2007, ApJ, 669, 1298; figure 10), which can be tested with better statistics of misaligned spin-orbit angles.
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