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Modeling of a Spot on τ Boötis A - Possibly Induced by a Planet

Dimitrov W., Tokarek J., Troianskyi V., Godunova V., Boneva D.

Acta Astronomica

2025

Vol. 75, No. 1

53--61

Photometry of τ Boötis A acquired by MOST satellite shows variations, which could be explained by the presence of a spot on the host star surface, potentially induced by its planetary companion. We used the Wilson-Devinney method for modeling the light curve. The results from the literature describing the star-planet system were used. Although τ Boötis is a non-transiting system, the masses, radii, and orbital inclination are known. The dominating factor in the light curve is the stellar spot effect. The ellipsoidal variations and reflected light influence are not visible or very small. Modeling shows a strong correlation between co-latitude and spot size. There is a group of solutions that fits the data well. If we suppose that the spot is on the star's equator we could find an unambiguous solution. The spot is shifted due to the sub-planetary point in the rotation direction. The longitude of the circular spot center is 62.°75±0.03. The temperature contrast of the spot is very low, only a few degrees below ambient temperature. The spots cover a significant part of the stellar surface, its radius is 56°±4. We also presented a second solution, which better fits the data, for a much smaller spot at latitude ≈30° and radius of 9.°7±0.1. The influence of light reflected from the day side of the planet was also analyzed.