We present a new model for E llipsoidal V ariations I nduced by a L ow- M ass C ompanion , the EVIL-MC model An IDL version of the model is publicly available at \href http : //www.lpl.arizona.edu/ bjackson/idl_code/index.htmlhttp : //www.lpl.arizona.edu/ \sim bjackson/idl_code/index.html . .
We employ several approximations appropriate for planetary systems to substantially increase the computational efficiency of our model relative to more general ellipsoidal variation models and improve upon the accuracy of simpler models .
This new approach gives us a unique ability to rapidly and accurately determine planetary system parameters .
We use the EVIL-MC model to analyze Kepler Quarter 0-2 ( Q0-2 ) observations of the HAT-P-7 system , an F-type star orbited by a \sim Jupiter-mass companion .
Our analysis corroborates previous estimates of the planet-star mass ratio q = ( 1.10 \pm 0.06 ) \times 10 ^ { -3 } , and we have revised the planet ’ s dayside brightness temperature to 2680 ^ { +10 } _ { -20 } K. We also find a large difference between the day- and nightside planetary flux , with little nightside emission .
Preliminary dynamical+radiative modeling of the atmosphere indicates this result is qualitatively consistent with high altitude absorption of stellar heating .
Similar analyses of Kepler and CoRoT photometry of other planets using EVIL-MC will play a key role in providing constraints on the properties of many extrasolar systems , especially given the limited resources for follow-up and characterization of these systems .
However , as we highlight , there are important degeneracies between the contributions from ellipsoidal variations and planetary emission and reflection .
Consequently , for many of the hottest and brightest Kepler and CoRoT planets , accurate estimates of the planetary emission and reflection , diagnostic of atmospheric heat budgets , will require accurate modeling of the photometric contribution from the stellar ellipsoidal variation .