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We observed nine primary transits of the hot Jupiter TrES-3b in severaloptical and near-UV photometric bands from 2009 June to 2012 April in anattempt to detect its magnetic field. Vidotto, Jardine and Helling suggest thatthe magnetic field of TrES-3b can be constrained if its near-UV light curveshows an early ingress compared to its optical light curve, while its egressremains unaffected. Predicted magnetic field strengths of Jupiter-like planetsshould range between 8 G and 30 G. Using these magnetic field values and anassumed B_star of 100 G, the Vidotto et al. method predicts a timing differenceof 5-11 min. We did not detect an early ingress in our three nights of near-UVobservations, despite an average cadence of 68 s and an average photometricprecision of 3.7 mmag. However, we determined an upper limit of TrES-3b'smagnetic field strength to range between 0.013 and 1.3 G (for a 1-100 Gmagnetic field strength range for the host star, TrES-3) using a timingdifference of 138 s derived from the Nyquist-Shannon sampling theorem. Toverify our results of an abnormally small magnetic field strength for TrES-3band to further constrain the techniques of Vidotto et al., we propose futureobservations of TrES-3b with other platforms capable of achieving a shorternear-UV cadence. We also present a refinement of the physical parameters ofTrES-3b, an updated ephemeris and its first published near-UV light curve. Wefind that the near-UV planetary radius of Rp = 1.386+0.248-0.144 RJup isconsistent with the planet's optical radius.

Near-UV and optical observations of the transiting exoplanet TrES-3b