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TYC 8241 2652 1 is a young star that showed a strong mid-infrared (mid-IR,8-25 mu) excess in all observations before 2008 consistent with a dusty disk.Between 2008 and 2010 the mid-IR luminosity of this system dropped dramaticallyby at least a factor of 30 suggesting a loss of dust mass of an order ofmagnitude or more. We aim to constrain possible models including removal ofdisk material by stellar activity processes, the presence of a binarycompanion, or other explanations suggested in the literature. We present newX-ray observations, optical spectroscopy, near-IR interferometry, and mid-IRphotometry of this system to constrain its parameters and further explore thecause of the dust mass loss. In X-rays TYC 8241 2652 1 has all propertiesexpected from a young star: Its luminosity is in the saturation regime and theabundance pattern shows enhancement of O/Fe. The photospheric Ha line is filledwith a weak emission feature, indicating chromospheric activity consistent withthe observed level of coronal emission. Interferometry does not detect acompanion and sets upper limits on the companion mass of 0.2, 0.35, 0.1 and0.05 M_sun at projected physical separations of 0.1-4 AU,4-5 AU, 5-10 AU, and10-30 AU, respectively (assuming a distance of 120.9 pc). Our mid-IRmeasurements, the first of the system since 2012, are consistent with thedepleted dust level seen after 2009. The new data confirms that stellaractivity is unlikely to destroy the dust in the disk and shows that scenarioswhere either TYC 8241 2652 1 heats the disk of a binary companion or apotential companion heats the disk of TYC 8241 2652 1 are unlikely.

TYC 8241 2652 1 and the case of the disappearing disk: no smoking gun yet